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

Analysing a large representative sample of local galaxies (8707), we findthat the variation in the shape of their dust attenuation curves is drivenprimarily by their structure, i.e., distribution of stars (and dust) withinthem. The attenuation curve for spheroid dominated galaxies, as compared to thedisc dominated ones, is nearly twice as steep. Both structural types coverdistinct ranges of attenuation slope values. Similar findings are reflected inthe case of star-forming and passive galaxies. Spheroids and passive galaxieswitness minimal attenuation in the optical compared to UV wavelengthsunderlining the lack of dusty birth-clouds that define complex star-dustgeometry. The distinction in the attenuation properties of spheroids and discsis maintained in each stellar mass range emphasising that structure is theprimal cause of variation. However, within a structural group, the attenuationcurve becomes shallower with both the increase in total stellar mass andoptical depth of the galaxy. Overall, with the extinction curve fixed to be thesame for all galaxies, the star-dust geometry emerges to be the primedeterminant of the variation in their attenuation properties.

Star-dust geometry main determinant of dust attenuation in galaxies