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Line identifications of type I supernovae: on the detection of Si II for these hydrogen-poor events

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dc.contributor.author Parrent, J. T
dc.contributor.author Milisavljevic, D
dc.contributor.author Soderberg, A. M
dc.contributor.author Parthasarathy, M
dc.date.accessioned 2020-11-19T13:45:20Z
dc.date.available 2020-11-19T13:45:20Z
dc.date.issued 2016-03
dc.identifier.citation The Astrophysical Journal, Vol. 820, No. 1, 75 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/7254
dc.description Restricted Access © The American Astronomical Society http://dx.doi.org/10.3847/0004-637X/820/1/75 en_US
dc.description.abstract Here we revisit line identifications of type I supernovae (SNe I) and highlight trace amounts of unburned hydrogen as an important free parameter for the composition of the progenitor. Most one-dimensional stripped-envelope models of supernovae indicate that observed features near 6000–6400 Å in typeI spectra are due to more than Si IIλ6355. However, while an interpretation of conspicuous Si IIλ6355 can approximate 6150 Å absorption features for all SNe Ia during the first month of free expansion, similar identifications applied to 6250 Å features of SNe Ib and Ic have not been as successful. When the corresponding synthetic spectra are compared with highquality timeseries observations, the computed spectra are frequently too blue in wavelength. Some improvement can be achieved with Fe II lines that contribute redward of 6150 Å; however, the computed spectra either remain too blue or the spectrum only reaches a fair agreement when the rise-time to peak brightness of the model conflicts with observations by a factor of two. This degree of disagreement brings into question the proposed explosion scenario. Similarly, a detection of strong Si IIλ6355 in the spectra of broadlined Ic and super-luminous events of type I/R is less convincing despite numerous model spectra used to show otherwise. Alternatively, we suggest 6000–6400 Å features are possibly influenced by either trace amounts of hydrogen or blueshifted absorption and emission in Hα, the latter being an effect which is frequently observed in the spectra of hydrogen-rich, SNe II. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Supernovae: general en_US
dc.title Line identifications of type I supernovae: on the detection of Si II for these hydrogen-poor events en_US
dc.type Article en_US


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