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

For a compiled sample of 120 reverberation-mapped AGNs, the bivariatecorrelations of the broad-line regions (BLRs) size ($R_{\rm BLR}$) with thecontinuum luminosity at 5100 \AA\ ($L_{5100}$) and the dimensionless accretionrates ($\dot{\mathscr{M}}$) are investigated. Using our recently calibratedvirial factor $f$, and the velocity tracer from the H$\beta$ Full-width athalf-maximum (FWHM(H$\beta$)) or the line dispersion ($\sigma_{\rm H\beta}$)measured in the mean spectra, three kinds of SMBH masses and$\dot{\mathscr{M}}$ are calculated. An extended \RL relation including$\dot{\mathscr{M}}$ is found to be stronger than the canonical $R_{\rmBLR}({\rm H\beta}) - L_{\rm 5100}$ relation, showing smaller scatters. Theobservational parameters, $R_{\rm Fe}$ (the ratio of optical Fe II to H$\beta$line flux) and the line profile parameter $D_{\rm H\beta}$ ($D_{\rm H\beta}=\rmFWHM(H\beta)/\sigma_{\rm H\beta}$), have relations with three kinds of$\dot{\mathscr{M}}$. Using $R_{\rm Fe}$ and $D_{\rm H\beta}$ to substitute$\dot{\mathscr{M}}$, extended empirical $R_{\rm BLR}({\rm H\beta}) - L_{\rm5100}$ relations are presented. $R_{\rm Fe}$ is a better "fix" for the $R_{\rmBLR}({\rm H\beta}) - L_{\rm 5100}$ offset than the H$\beta$ shape $D_{\rmH\beta}$. The extended empirical $R_{\rm BLR}({\rm H\beta}) - L_{\rm 5100}$relation including $R_{\rm Fe}$ can be used to calculate $R_{\rm BLR}$, andthus the single-epoch SMBH mass $M_{\rm BH}$. Our measured accretion ratedependence is not consistent with the simple model of the accretion diskinstability leading the BLRs formation. The BLR may instead form from the inneredge of the torus, or from some other means in which BLR size is positivelycorrelated with accretion rate and the SMBH mass.

An extended size-luminosity relation for the reverberation-mapped AGNs: the role of the accretion rate