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 have carried out optical observations of the north-eastern part of thesupernova remnant IC 443 using the CFHT imaging spectrograph SITELLE. Theobservations consist of three multispectral cubes covering an 11$^{\prime}$$\times$11$^{\prime}$ area allowing the investigation of both the spatial andspectral variation of 9 emission lines : [OII] $\lambda\lambda$3726+3729,[OIII] $\lambda\lambda$4959,5007, H$\beta$, H$\alpha$, [NII]$\lambda\lambda$6548,6583 and [SII] $\lambda\lambda$6716,6731. Extinctionmeasurement from the H$\alpha$ / H$\beta$ ratio shows significant variationacross the observed region with E(B-V) = 0.8-1.1. Electron density measurementsusing [SII] lines indicate densities ranging from 100 up to 2500 cm$^{-3}$.Models computed with the shock modelling code MAPPINGS are presented andcompared with the observations. A combination of complete shock model andtruncated ones are required in order to explain the observed spectrum. Theshock velocities found in IC 443 are between 20 and 150 km/s with 75 km/s beingthe most prominent velocity. The pre-shock number density varies from 20 to 60cm$^{-3}$. A single set of abundances close to solar values combined withvarying shock parameters (shock velocity, pre-shock density and shock age) aresufficient to explain to great variation of lines intensities observed in IC443. Despite the relatively modest spectral resolution of the data (R$\sim1500$ at H$\alpha$), we clearly separate the red and blue velocity componentsof the expanding nebula, which show significant morphological differences.

A multispectral analysis of the northeastern shell of IC 443