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 high-resolution hydrodynamic simulation that tracks thenon-equilibrium abundance of molecular hydrogen within a massive high-redshiftgalaxy to produce mock Atacama Large Millimeter Array (ALMA) maps of thefine-structure lines of atomic carbon, CI 1-0 and CI 2-1. Inspired by recentobservational and theoretical work, we assume that CI is thoroughly mixedwithin giant molecular clouds and demonstrate that its emission is an excellentproxy for H2. Nearly all of the H2 associated with the galaxy can be detectedat redshifts z<4 using a compact interferometric configuration with a largesynthesized beam (that does not resolve the target galaxy) in less than 4 h ofintegration time. Low-resolution imaging of the \CI lines (in which the targetgalaxy is resolved into three to four beams) will detect ~80 per cent of the H2in less than 12 h of aperture synthesis. In this case, the resulting data cubealso provides the crucial information necessary for determining the dynamicalstate of the galaxy. We conclude that ALMA observations of the CI 1-0 and 2-1emission are well-suited for extending the interval of cosmic look-back timeover which the H2 distributions, the dynamical masses, and the Tully-Fisherrelation of galaxies can be robustly probed.

Atomic carbon as a powerful tracer of molecular gas in the high-redshift Universe: perspectives for ALMA