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 model the evolution of active galactic nuclei by constructing their radioluminosity functions. We use a set of surveys of varying area and depth, namelythe deep COSMOS survey of $1,916$ AGN sources, the wide shallow 3CRR, 7C and6CE surveys, containing together $356$ AGNs, and the intermediate XXL-North andSouth fields consisting of $899$ and $1,484$ sources, respectively. We alsoused the CENSORS, BRL, Wall $\&$ Peacock and Config surveys, consistingrespectively of $150$, $178$, $233$ and $230$ sources. Together, these surveysnumbered $5,446$ AGN sources and constrained the luminosity functions at highredshift and over a wide range of luminosities (up to $z \approx 3$ and $\log(L / \mathrm{W Hz^{-1}}) \in [22,29])$. We concentrate on parametric methodswithin the Bayesian framework and show that the luminosity-dependent densityevolution (LDDE) model fits the data best, with evidence ratios varying from"strong" ($>10$) to "decisive" ($>100$) according to the Jeffreysinterpretation. We determine the number density, luminosity density and kineticluminosity density as a function of redshift, and observe a flattening of thesefunctions at higher redshifts, not present in simpler models, which we explainby our use of the LDDE model. Finally, we divide our sample into subsetsaccording to the stellar mass of the host galaxies in order to investigate apossible bimodality in evolution. We found a difference in LF shape andevolution between these subsets. All together, these findings point to aphysical picture where the evolution and density of AGN cannot be explainedwell by simple models but require more complex models either via AGNsub-populations where the total AGN sample is divided into subsamples accordingto various properties such as, for example, optical properties and stellarmass, or via luminosity-dependent functions.

The XXL survey LII : The evolution of radio AGN luminosity function  determined via parametric methods from GMRT, ATCA, VLA and Cambridge  interferometer observations