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 study the relationship between the [CII] emission and the star formationrate (SFR) in the Galactic plane and separate the relationship of different ISMphases to the SFR. We compare these relationships to those in external galaxiesand local clouds, allowing examinations of these relationships over a widerange of physical scales. We compare the distribution of the [CII] emission,with its different contributing ISM phases, as a function of Galactocentricdistance with the SFR derived from radio continuum observations. We alsocompare the SFR with the surface density distribution of atomic and moleculargas, including the CO-dark H2 component. The [CII] and SFR are well correlatedat Galactic scales with a relationship that is in general agreement with thatfound for external galaxies. By combining [CII] and SFR data points in theGalactic plane with those in external galaxies and nearby star forming regions,we find that a single scaling relationship between the [CII] luminosity and SFRapplies over six orders of magnitude. The [CII] emission from different ISMphases are each correlated with the SFR, but only the combined emission shows aslope that is consistent with extragalactic observations. These ISM componentshave roughly comparable contributions to the Galactic [CII] luminosity: densePDRs (30%), cold HI (25%), CO-dark H2 (25%), and ionized gas (20%). The SFR-gassurface density relationship shows a steeper slope compared to that observed ingalaxies, but one that it is consistent with those seen in nearby clouds. Thedifferent slope is a result of the use of a constant CO-to-H2 conversion factorin the extragalactic studies, which in turn is related to the assumption ofconstant metallicity in galaxies. We find a linear correlation between the SFRsurface density and that of the dense molecular gas.

A Herschel [CII] Galactic plane survey III: [CII] as a tracer of star formation