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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We present the first characterisation of the average dust attenuation curveat $z\sim1.3$ by combining rest-frame ultraviolet through near-IR photometrywith Balmer decrement ($\mathrm{H}\alpha$/$\mathrm{H}\beta$) constraints for$\sim$900 galaxies with $8\lesssim\log (M_\star /M_\odot)<10.2$ at $0.75<z<1.5$in the HST WFC3 IR Spectroscopic Parallel (WISP) and 3D-HST grism surveys.Using galaxies in SDSS, we establish that the ($\mathrm{H}\alpha$+[NII])/[OIII]line ratio and stellar mass are good proxies for the Balmer decrement inlow-spectral resolution grism data when only upper-limits on $\mathrm{H}\beta$are available and/or $\mathrm{H}\alpha$ is blended with [NII]. The slope of the$z\sim1.3$ attenuation curve ($A(0.15\mu m)/A(V)=3.15$) and its normalization($R_V=3.26$) lie in-between the values found for $z=0$ and $z\sim2$ dustattenuation curves derived with similar methods. These provide supportingevidence that the average dust attenuation curve of star forming galaxiesevolves continuously with redshift. The $z\sim1.3$ curve has a mild 2175\r{A}feature (bump amplitude, $E_b=0.83$; $\sim$25% that of the MW extinctioncurve), which is comparable to several other studies at $0<z\lesssim3$, andsuggests that the average strength of this feature may not evolve significantlywith redshift. The methods we develop to constrain dust attenuation from HSTgrism data can be applied to future grism surveys with JWST, Euclid, and RST.These new facilities will detect millions of emission line galaxies and offerthe opportunity to significantly improve our understanding of how and why dustattenuation curves evolve.

The average dust attenuation curve at z~1.3 based on HST grism surveys