SN 2019hcc: A Type II supernova displaying early O ii lines

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dc.contributor.authorParrag, Eleonora
dc.contributor.authorInserra, Cosimo
dc.contributor.authorSchulze, Steve
dc.contributor.authorAnderson, Joseph
dc.contributor.authorChen, Ting-Wan
dc.contributor.authorLeloudas, Giorgios
dc.contributor.authorGalbany, Lluis
dc.contributor.authorGutiérrez, Claudia P.
dc.contributor.authorHiramatsu, Daichi
dc.contributor.authorKankare, Erkki
dc.contributor.authorMüller-Bravo, Tomás E.
dc.contributor.authorNicholl, Matt
dc.contributor.authorPignata, Giuliano
dc.contributor.authorCartier, Regis
dc.contributor.authorGromadzki, Mariusz
dc.contributor.authorKozyreva, Alexandra
dc.contributor.authorRau, Arne
dc.contributor.authorBurke, Jamison
dc.contributor.authorHowell, D. Andrew
dc.contributor.authorMccully, Curtis
dc.contributor.authorPellegrino, Craig
dc.date.accessioned2025-04-08T14:52:38Z
dc.date.available2025-04-08T14:52:38Z
dc.date.issued2021-10
dc.descriptionIndexación: Scopus.
dc.description.abstractWe present optical spectroscopy together with ultraviolet, optical, and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a 'w' shape at around 4000 Å which is usually associated with O ii lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed H α P-Cygni profile from 19 d past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supernova (SN IIL). The object does not show any unambiguous sign of interaction as there is no evidence of narrow lines in the spectra or undulations in the light curve. Our tardis spectral modelling of the first spectrum shows that carbon, nitrogen, and oxygen (CNO) at 19 000 K reproduce the 'w' shape and suggests that a combination of non-thermally excited CNO and metal lines at 8000 K could reproduce the feature seen at 4000 Å. The Bolometric light-curve modelling reveals that SN 2019hcc could be fit with a magnetar model, showing a relatively strong magnetic field (B > 3 × 1014 G), which matches the peak luminosity and rise time without powering up the light curve to superluminous luminosities. The high-energy photons produced by the magnetar would then be responsible for the detected O ii lines. As a consequence, SN 2019hcc shows that a 'w' shape profile at around 4000 Å, usually attributed to O ii, is not only shown in superluminous supernovae and hence it should not be treated as the sole evidence of the belonging to such a supernova type. © 2021 The Author(s).
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/506/4/4819/6324586
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Volume 506, Issue 4, Pages 4819 - 4840, 1 October 2021
dc.identifier.doi10.1093/mnras/stab2074
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/handle/ria/64018
dc.language.isoen
dc.publisherOxford University Press
dc.rights.licenseAttribution 4.0 International CC BY 4.0 Deed
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/
dc.subjectLine: Formation
dc.subjectLine: Identification
dc.subjectStars: Magnetars
dc.titleSN 2019hcc: A Type II supernova displaying early O ii lines
dc.typeArtículo
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