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 use a sample of 706 galaxies, selected as [OII]$\lambda$3727 ([OII])emitters in the Survey for High-$z$ Absorption Red and Dead Sources (SHARDS) onthe CANDELS/GOODS-N field, to study the differential attenuation of the nebularemission with respect to the stellar continuum. The sample includes onlygalaxies with a counterpart in the infrared and$\mathrm{log}_{10}(M_{*}/\mathrm{M}_{\odot})$ $>$ 9, over the redshift interval0.3 $\lesssim$ $z$ $\lesssim$ 1.5. Our methodology consists in the comparisonof the star formation rates inferred from [OII] and H$\alpha$ emission lineswith a robust quantification of the total star-forming activity(${SFR}_{\mathrm{TOT}}$) that is independently estimated based on both infraredand ultraviolet (UV) luminosities. We obtain$f$$=$$E(B-V)_{\mathrm{stellar}}$/$E(B-V)_{\mathrm{nebular}}$ $=$0.69$^{0.71}_{0.69}$ and 0.55$^{0.56}_{0.53}$ for [OII] and H$\alpha$,respectively. Our resulting $f$-factors display a significant positivecorrelation with the UV attenuation and shallower or not-significant trendswith the stellar mass, the $SFR_{\mathrm{TOT}}$, the distance to the mainsequence, and the redshift. Finally, our results favour an average nebularattenuation curve similar in shape to the typical dust curve of localstarbursts.

Differential attenuation in star-forming galaxies at 0.3 $\lesssim$ $z$ $\lesssim$ 1.5 in the SHARDS/CANDELS field