Kavli Affiliate: Luis C. Ho
| First 5 Authors: Yijun Wang, Tao Wang, Luis C. Ho, Yuxing Zhong, Bin Luo
| Summary:
The fundamental plane of back hole activity (BHFP) describes the correlation
between radio luminosity ($L_R$), X-ray luminosity ($L_X$), and black hole mass
($M_{BH}$). It reflects a connection between accretion disc and jet. However,
the dependence of the BHFP on various physical properties of active galactic
nuclei (AGNs) and host galaxies remains unclear, especially for low-luminosity
AGNs. From the deep and large multi-wavelength surveys in the GOODS-N, GOODS-S,
and COSMOS/UltraVISTA fields, we constructed a large and homogeneous radio AGN
sample including 208 objects. We divided this sample into 141 radio-quiet (RQ)
AGNs and 67 radio-loud (RL) AGNs according to the radio-loudness defined by the
ratio of $L_R$ to $L_X$. The $L_R$-to-$L_X$ ratio shows a bimodal distribution
that is well described by two single Gaussian models. Their cross point
corresponds to a radio-loudness threshold of $log (L_R/L_X)=-2.73$. The RQ
AGNs have larger Eddington ratio ($lambda_{Edd}$) than the RL AGNs. Our RQ and
RL AGNs show different BHFPs that are $log L_R=(0.55pm 0.05)log L_X+(0.28pm
0.06)log M_{BH}+(13.54pm 2.27)$ and $log L_R=(0.82pm 0.08)log L_X+(0.07pm
0.08)log M_{BH}+(5.24pm 3.33)$, respectively. For both RQ and RL AGNs, the
BHFP does not show a significant dependence on redshift and galaxy
star-formation properties, while it shows a significant dependence on
$lambda_{Edd}$. The BHFP sheds important light on the accretion physics of
central engines. RQ AGNs at $0.01<lambda_{Edd}<0.1$ agree with the advection
dominated accretion flow (ADAF) coupled with a synchrotron jet model, while at
$0.1<lambda_{Edd}< 1$, they mainly follow the jet model. RL AGNs are
consistent with a combination of ADAF and jet model at $lambda_{Edd}<0.01$,
and agree with the jet model at $0.01<lambda_{Edd}<0.1$, and follow a
combination of the standard thin disc and jet model at $lambda_{Edd}>0.1$.
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