SN 2020cpg: an energetic link between Type IIb and Ib supernovae
| Autor: | Jesper Sollerman, Matt Nicholl, Erkki Kankare, Lluís Galbany, Mariusz Gromadzki, Cosimo Inserra, Paolo A. Mazzali, Claudia P. Gutiérrez, M Amenouche, J. Teffs, D. A. Howell, T. E. Müller-Bravo, Jamison Burke, Tao Chen, Daichi Hiramatsu, C. Ashall, Joseph P. Anderson, K Medler, C. Pellegrino, Curtis McCully, S. J. Prentice |
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| Přispěvatelé: | Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA) |
| Jazyk: | angličtina |
| Rok vydání: | 2021 |
| Předmět: |
Stripping (chemistry)
Hydrogen Astrophysics::High Energy Astrophysical Phenomena general [Supernovae] chemistry.chemical_element FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics Kinetic energy 01 natural sciences Luminosity supernovae: individual (SN 2020cpg) supernovae: general 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Ejecta 010303 astronomy & astrophysics QC Astrophysics::Galaxy Astrophysics QB Envelope (waves) Physics High Energy Astrophysical Phenomena (astro-ph.HE) 010308 nuclear & particles physics individual (SN 2020cpg) [Supernovae] Astronomy and Astrophysics Light curve Supernova chemistry 13. Climate action Space and Planetary Science Astrophysics - High Energy Astrophysical Phenomena [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] |
| Zdroj: | Monthly Notices of the Royal Astronomical Society Monthly Notices of the Royal Astronomical Society, 2021, 506 (2), pp.1832-1849. ⟨10.1093/mnras/stab1761⟩ Mon.Not.Roy.Astron.Soc. Mon.Not.Roy.Astron.Soc., 2021, 506 (2), pp.1832-1849. ⟨10.1093/mnras/stab1761⟩ Digibug. Repositorio Institucional de la Universidad de Granada Consorcio Madroño |
| ISSN: | 0035-8711 1365-2966 |
| Popis: | S.J. Prentice is supported by H2020 ERC grant no. 758638. J.J. Teffs is funded by the consolidated STFC grant no. R27610. This paper is based in part on observations collected at the European Southern Observatory (ESO) under ESO programme 1103.D-0328(J). T.W. Chen acknowledges the European Union Funding under Marie Sklodowska-Curie grant no. H2020-MSCA-IF-2018-842471. L. Galbanywas funded by the European Union'sHorizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant no. 839090. This work has been partially supported by the Spanish grant no. PGC2018-095317-B-C21 within the European Funds for Regional Development (FEDER). M. Gromadzki is supported by the Polish National Science Center (NCN) MAESTRO grant no. 2014/14/A/ST9/00121. T. M uller-Bravo was funded by the CONICYT PFCHA/DOCTORADOBECAS CHILE/2017-72180113. M. Nicholl is supported by a Royal Astronomical Society Research Fellowship. Thiswork makes use of observations obtained by the Las Cumbres Observatory global telescope network. The LCO team is supported by NSF grant nos AST-1911225 and AST-1911151. Based in part on observations made with the Liverpool Telescope operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Institutode Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council. The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de As-trofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA, with observation having been made with the Nordic Optical Telescope, operated at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. ATLAS is primarily funded to search for near earth asteroids through NASA grant nos NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; by-products of the NEO search include images and catalogues from the survey area. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen's University Belfast, and the Space Telescope Science Institute. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+(the advanced Public ESO Spectroscopic Survey for Transient Objects Survey). ePESSTO + observations were obtained under ESO programme ID 1103.D-0328 (PI: Inserra). LCO data have been obtained via OPTICON proposals (IDs: SUPA2020B-002 SUPA2020A-001 OPTICON 20A/015 and OPTICON 20B/003). The OPTICON project has received funding from the European Union's Horizon 2020 research and innovation programme under grant no. 730890. Stripped-envelope supernovae (SE-SNe) show a wide variety of photometric and spectroscopic properties. This is due to the different potential formation channels and the stripping mechanism that allows for a large diversity within the progenitors outer envelope compositions. Here, the photometric and spectroscopic observations of SN 2020cpg covering ∼130 d from the explosion date are presented. SN 2020cpg (z = 0.037) is a bright SE-SNe with the B-band peaking at MB = −17.75 ± 0.39 mag and a maximum pseudo-bolometric luminosity of Lmax = 6.03 ± 0.01 × 1042 erg s−1. Spectroscopically, SN2020cpg displays a weak high- and low-velocity H α feature during the photospheric phase of its evolution, suggesting that it contained a detached hydrogen envelope prior to explosion. From comparisons with spectral models, the mass of hydrogen within the outer envelope was constrained to be ∼0.1 M . From the pseudo-bolometric light curve of SN 2020cpg a 56Ni mass of MNi ∼ 0.27 ± 0.08M was determined using an Arnett-like model. The ejecta mass and kinetic energy of SN 2020cpg were determined using an alternative method that compares the light curve of SN 2020cpg and several modelled SE-SNe, resulting in an ejecta mass of Mejc ∼ 5.5 ± 2.0 M and a kinetic energy of EK ∼ 9.0 ± 3.0 × 1051 erg. The ejected mass indicates a progenitor mass of 18−25 M . The use of the comparative light curve method provides an alternative process to the commonly used Arnett-like model to determine the physical properties of SE-SNe. H2020 ERC 758638 UK Research & Innovation (UKRI) Science & Technology Facilities Council (STFC) R27610 European Southern Observatory (ESO) 1103.D-0328(J) European Commission H2020-MSCA-IF-2018-842471 839090 730890 PGC2018-095317-B-C21 Polish National Science Center (NCN) MAESTRO 2014/14/A/ST9/00121 CONICYT PFCHA/DOCTORADOBECAS CHILE/2017-72180113 Royal Astronomical Society Research Fellowship National Science Foundation (NSF) AST-1911225 AST-1911151 Science & Technology Facilities Council (STFC) National Aeronautics & Space Administration (NASA) NN12AR55G 80NSSC18K0284 80NSSC18K1575 ESO programme 1103.D-0328 |
| Databáze: | OpenAIRE |
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