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

Given the multiple energy loss mechanisms of cosmic ray electrons ingalaxies, the tightness of the infrared - radio continuum correlation issurprising. We extended the analytical model of galactic disks of Vollmer etal. (2017) by including a simplified prescription for the synchrotronemissivity. The galactic gas disks of local spiral galaxies, low-z starburstgalaxies, high-z main sequence starforming, and high-z starburst galaxies aretreated as turbulent clumpy accretion disks. The magnetic field strength isdetermined by the equipartition between the turbulent kinetic and the magneticenergy densities. Our fiducial model, which neither includes galactic winds norCR electron secondaries, reproduces the observed radio continuum SEDs of most(~70%) of the galaxies. Except for the local spiral galaxies, fast galacticwinds can potentially make the conflicting models agree with observations. Theobserved IR - radio correlations are reproduced by the model within 2 sigma ofthe joint uncertainty of model and data for all datasets. The model agrees withthe observed SFR - radio correlations within ~4 sigma. Energy equipartitionbetween the CR particles and the magnetic field only approximately holds in ourmodels of main sequence starforming galaxies. If a CR electron calorimeter isassumed, the slope of the IR - radio correlation flattens significantly.Inverse Compton (IC) losses are not dominant in the starburst galaxies becausein these galaxies not only the gas density but also the turbulent velocitydispersion is higher than in normally starforming galaxies. Equipartitionbetween the turbulent kinetic and magnetic field energy densities then leads tovery high magnetic field strengths and very short synchrotron timescales. Theexponents of our model SFR - radio correlations at 150 MHz and 1.4 GHz are veryclose to one.

astronomy and astrophysics

Deciphering the radio star formation correlation on kpc scales II. The  integrated infrared-radio continuum and star formation - radio continuum  correlations