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

The absence of high Eddington ratio, obscured Active Galactic Nuclei (AGN) inlocal ($z\lesssim0.1$) samples of moderate luminosity AGN has generally beenexplained to result from radiation pressure on the dusty gas governing thelevel of nuclear ($\lesssim10$pc) obscuration. However, very high accretionrates are routinely reported among obscured quasars at higher luminosities, andmay require a different feedback mechanism. We compile constraints onobscuration and Eddington ratio for samples of X-ray, optical, infrared, andsubmm selected AGN at quasar luminosities. Whereas moderate luminosity,obscured AGN in the local universe have a range of lower Eddington ratios($f_{\rm Edd} \sim 0.001-0.1$), the most luminous ($L_{\rm bol} \gtrsim 10^{46}$erg s$^{-1}$) IR/submm-bright, obscured quasars out to $z\sim3$ commonly havevery high Eddington ratios ($f_{\rm Edd} \sim 0.1-1$). This apparent lack ofradiation pressure feedback in luminous obscured quasars is likely coupled withAGN timescales, such that a higher fraction of luminous obscured quasars areseen due to the short timescale for which quasars are most luminous. Adoptingquasar evolutionary scenarios, extended ($\sim10^{2-3}$pc) obscuration may worktogether with the shorter timescales to explain the observed fraction ofobscured, luminous quasars, while outflows driven by radiation pressure willslowly clear this material over the AGN lifetime.

The Dust-to-Gas Ratio and the Role of Radiation Pressure in Luminous, Obscured Quasars