Observations of the very young Type Ia Supernova 2019np with early-excess emission

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dc.contributor.authorSai, Hanna
dc.contributor.authorWang, Xiaofeng
dc.contributor.authorElias Rosa, Nancy
dc.contributor.authorYang, Yi
dc.contributor.authorZhang, Jujia
dc.contributor.authorLin, Weili
dc.contributor.authorMo, Jun
dc.contributor.authorPiro, Anthony L
dc.contributor.authorZeng, Xiangyun
dc.contributor.authorAndrea, Reguitti
dc.contributor.authorBrown, Peter
dc.contributor.authorBurns, Christopher R
dc.contributor.authorCai, Yongzhi
dc.contributor.authorFiore, Achille
dc.contributor.authorHsiao, Eric Y
dc.contributor.authorIsern, Jordi
dc.contributor.authorItagaki, K.
dc.contributor.authorLi, Wenxiong
dc.contributor.authorLi, Zhitong
dc.contributor.authorPessi, Priscila J
dc.contributor.authorPhillips, M.M.
dc.contributor.authorSchuldt, Stefan
dc.contributor.authorShahbandeh, Melissa
dc.contributor.authorStritzinger, Maximilian D
dc.contributor.authorTomasella, Lina
dc.contributor.authorVogl, Christian
dc.contributor.authorWang, Bo
dc.contributor.authorWang, Lingzhi
dc.contributor.authorWu, Chengyuan
dc.contributor.authorYang, Sheng
dc.contributor.authorZhang, Jicheng
dc.contributor.authorZhang, Tianmeng
dc.contributor.authorZhang, Xinghan
dc.date.accessioned2023-11-06T17:53:29Z
dc.date.available2023-11-06T17:53:29Z
dc.date.issued2022-08-01
dc.descriptionIndexación: Scopus.es
dc.description.abstractEarly-time radiative signals from Type Ia supernovae (SNe Ia) can provide important constraints on the explosion mechanism and the progenitor system. We present observations and analysis of SN 2019np, a nearby SN Ia discovered within 1-2 days after the explosion. Follow-up observations were conducted in optical, ultraviolet, and near-infrared bands, covering the phases from ∼-16.7 d to ∼+ 367.8 d relative to its B-band peak luminosity. The photometric and spectral evolutions of SN 2019np resemble the average behaviour of normal SNe Ia. The absolute B-band peak magnitude and the post-peak decline rate are Mmax(B) =-19.52 ± 0.47 mag and Δm15(B) = 1.04 ± 0.04 mag, respectively. No Hydrogen line has been detected in the nebular-phase spectra of SN 2019np. Assuming that the 56Ni powering the light curve is centrally located, we find that the bolometric light curve of SN 2019np shows a flux excess up to 5.0 per cent in the early phase compared to the radiative diffusion model. Such an extra radiation perhaps suggests the presence of an additional energy source beyond the radioactive decay of central nickel. Comparing the observed colour evolution with that predicted by different models, such as interactions of SN ejecta with circumstellar matter (CSM)/companion star, a double-detonation explosion from a sub-Chandrasekhar mass white dwarf (WD) and surface 56Ni mixing, we propose that the nickel mixing is more favoured for SN 2019np. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.es
dc.description.urihttps://academic-oup-com.recursosbiblioteca.unab.cl/mnras/article/514/3/3541/6598822
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Volume 514, Issue 3, Pages 3541 - 3558, 1 August 2022es
dc.identifier.doi10.1093/mnras/stac1525
dc.identifier.issn0035-8711
dc.identifier.urihttps://repositorio.unab.cl/xmlui/handle/ria/53844
dc.language.isoenes
dc.publisherOxford University Presses
dc.rights.licenseCC BY 4.0 DEED Atribución 4.0 Internacional
dc.rights.urihttps://creativecommons.org/licenses/by/4.0/deed.es
dc.subjectSupernovae: generales
dc.subjectSupernovae: individual: (SN 2019np)es
dc.subjectInfrared deviceses
dc.subjectMixinges
dc.subjectNickeles
dc.subjectNickel compoundses
dc.subjectWhite dwarfses
dc.titleObservations of the very young Type Ia Supernova 2019np with early-excess emissiones
dc.typeArtículoes
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