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

JWST/NIRSpec is providing sensitive spectroscopic observations of distantgalaxies, extending our view of cosmic chemical evolution out to the epoch ofreionization and down to galaxy masses 1-2 dex lower than previously possibleat $z>2$. These observations nevertheless remain heavily dominated by lightfrom luminous star forming regions. An alternative and sensitive probe of themetallicity of galaxies is through absorption lines imprinted on the luminousafterglow spectra of long gamma ray burst (GRBs) from intervening materialwithin their host galaxy. However, these two independent but complementaryprobes need to be cross-calibrated before they can be combined. We present thefirst results from a cycle-1 JWST program to investigate the relation betweenthe metallicity of the neutral gas measured with GRB afterglow absorption linesto the emission line metallicity of the star forming regions of the GRB hostmeasured with NIRSpec. Using an initial sample of seven GRB host galaxies at$z=2-4$, we find a tight relation between absorption and emission linemetallicities when using the recent Laseter et al. (2023) $\hat{R}$ metallicitydiagnostic, implying a relatively chemically-homogeneous multi-phaseinterstellar medium, and indicating that absorption and emission line probescan be directly combined to investigate the chemical enrichment of galaxies.However, the relation is less clear when using other diagnostics, such as$R_{23}$ and $R_3$. Ultimate confirmation of the relation between absorptionand emission line metallicities will require a more direct determination of theemission line metallicity via the detection of temperature-sensitive aurorallines in our GRB host galaxy sample.

Comparing emission- and absorption-based gas-phase metallicities in GRB host galaxies at $z=2-4$ using JWST