English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We construct spectra of supernovae interacting strongly with a circumstellarmedium (CSM) by adding SN templates, a black-body continuum and anemission-line spectrum. In a Monte Carlo simulation we generate more than 800spectra, distribute them to 10 different classifiers and study how thedifferent simulation parameters affect the appearance of the spectra. SNe IInshowing some structure over the continuum were characterized as SNe IInS. Wedemonstrate that the flux ratio of the underlying SN to the continuum fv is themost important parameter determining the spectral classification. ThermonuclearSNe get progressively classified as Ia-CSM, IInS and IIn as fv decreases. Thetransition between Ia-CSM and IInS occurs at fv~0.2-0.3. It shown that SNeIa-CSM are found at the magnitude range -19.5> M >-21.6, in good agreement withobservations, and that the faintest SN IIn that can hide a SN Ia has M = -20.1.The sample of SNe Ia-CSM shows an association with 91T-like SNe Ia. Ourexperiment does not support that this association is due to a luminosity bias(91T-like being brighter than normal Ia). We therefore conclude that thisassociation has real physical origins and we propose that 91T-like explosionsresult from single degenerate progenitors. Despite the similarities between SNeIbc and SNe Ia, the number of misclassifications between these types was smalland mostly at low S/N. Combined with the luminosity function needed toreproduce the observed SN Ia-CSM luminosities, it is unlikely that SNe Ibcconstitute an important contaminant within this sample. We show how Type IIspectra transition to IIn and how the Ha profiles vary with fv. SNe IIn fainterthan M = -17.2 are unable to mask SNe IIP brighter than M = -15. A simulationincluding radiative transfer shows that our simplified model is a good firstorder approximation. The spectra obtained are in good agreement with real data.

Supernova spectra below strong circum-stellar interaction