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

A fundamental question in galaxy and black-hole evolution remains howgalaxies and their supermassive black holes have evolved together over cosmictime. Specifically, it is still unclear how the position of X-ray activegalactic nucleus (AGN) host galaxies with respect to the star-forming mainsequence (MS) may change with the X-ray luminosity ($L_\mathrm{X}$) of the AGNor the stellar mass ($M_\star$) of the host galaxy. We use data from XMM-SERVSto probe this issue. XMM-SERVS is covered by the largest medium-depth X-raysurvey (with superb supporting multiwavelength data) and thus contains thelargest sample to date for study. To ensure consistency, we locally derive theMS from a large reference galaxy sample. In our analysis, we demonstrate thatthe turnover of the galaxy MS does not allow reliable conclusions to be drawnfor high-mass AGNs, and we establish a robust safe regime where the results donot depend upon the choice of MS definition. Under this framework, our resultsindicate that less-massive AGN host-galaxies ($\log M_\star\sim9.5-10.5$$M_\odot$) generally possess enhanced SFRs compared to their normal-galaxycounterparts while the more-massive AGN host galaxies ($\logM_\star\sim10.5-11.5$ $M_\odot$) lie on or below the star-forming MS. Further,we propose an empirical model for how the placement of an AGN with respect tothe MS (SFR$_{norm}$) evolves as a function of both $M_\star$ and$L_\mathrm{X}$.

Investigating the Star Formation Rates of AGN Hosts Relative to the Star-Forming Main Sequence