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 new Band-3 CO(1-0) observations taken with the Atacama LargeMillimeter/submillimeter Array (ALMA) to study the physical conditions in theinterstellar gas of a sample of 27 dusty main-sequence star-forming galaxies at0.03<$z$<0.2 present in the Valpara\'iso ALMA Line Emission Survey (VALES). Thesample is drawn from far-IR bright galaxies over $\sim$160 deg$^{2}$ in theHerschel Astrophysical Terahertz Large Area Survey (HATLAS), which is coveredby Herschel [CII] 158 $\mu$m spectroscopy and far-infrared (FIR) photometry.The [CII] and CO lines are both detected at >5$\sigma$ in 26 sources. We findan average [CII] to CO(1-0) luminosity ratio of 3500$\pm$1200 for our samplethat is consistent with previous studies. Using the [CII], CO and FIRmeasurements as diagnostics of the physical conditions of the interstellarmedium, we compare these observations to the predictions of a photodissociationregion (PDR) model to determine the gas density, surface temperature, pressure,and the strength of the incident far-ultraviolet (FUV) radiation field,$G_{0}$, normalised to the Habing Field. The majority of our sample exhibithydrogen densities of 4 < $\log n/\mathrm{cm}^{3}$ < 5.5 and experience anincident FUV radiation field with strengths of 2 < $\log G_0$ < 3 when adoptingstandard adjustments. A comparison to galaxy samples at different redshiftsindicates that the average strength of the FUV radiation field appears constantup to redshift $z\sim$6.4, yet the neutral gas density increases with redshiftby a factor of $\sim$100, that persists regardless of various adjustments toour observable quantities. This evolution could provide an explanation for theobserved evolution of the star formation rate density with cosmic time, yetcould arise from a combination of observational biases when using differentsuites of emission lines as diagnostic tracers of PDR gas.

VALES: II. The physical conditions of interstellar gas in normal star-forming galaxies up to z=0.2 revealed by ALMA