NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-18 T02:55:27 PDT
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For refcode 2015MNRAS.453.3447D:
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Copyright by Royal Astronomical Society. 2015MNRAS.453.3447D Revisit the Fundamental Plane of black hole activity from sub-Eddington to quiescent state Dong, Ai-Jun; Wu, Qingwen Abstract. It is very controversial whether radio-X-ray correlation as defined in low-hard state of X-ray binaries (XRBs) can extend to quiescent state (e.g. X-ray luminosity less than a critical value of L_X,c_ ~ 10^-5.5^L_Edd_) or not. In this work, we collect a sample of XRBs and low-luminosity active galactic nuclei (LLAGNs) with wide distribution of Eddington ratios (L_X_/L_Edd_ ~ 10^-9^-10^-3^) to re-explore the Fundamental Plane between 5 GHz radio luminosity, L_R_, 2-10 keV X-ray luminosity, L_X_, and black hole (BH) mass, M_BH_, namely log L_R_ = xi_X_log L_X_ + xi_M_log M_BH_ + constant. For the whole sample, we confirm the former Fundamental Plane of Merloni et al. and Falcke et al. that xi_X_ ~ 0.6 and xi_M_ ~ 0.8 even after including more quiescent BHs. The quiescent BHs follow the Fundamental Plane very well, and, however, FR I radio galaxies follow a steeper track comparing other BH sources. After excluding FR Is, we investigate the Fundamental Plane for BHs in quiescent state with L_X_ < L_X,c_ and sub-Eddington BHs with L_X_ > L_X,c_, respectively, and both sub-samples have a similar slope, xi_X_ ~ 0.6, which support that quiescent BHs may behave similar to those in low-hard state. We further select two sub-samples of AGNs with BH mass in a narrow range (FR Is with M_BH_ = 10^8.8+/-0.4^ and other LLAGNs with M_BH_ = 10^8.0+/-0.4^) to simulate the behaviour of a single supermassive BH evolving from sub-Eddington to quiescent state. We find that the highly sub-Eddington sources with L_X_/L_Edd_ ~ 10^-6^-10^-9^ still roughly stay on the extension of radio-X-ray correlation as defined by other sub-Eddington BHs. Our results are consistent with several recent observations in XRBs that the radio-X-ray correlation as defined in low-hard state can extend to highly sub-Eddington quiescent state. Key words: accretion, accretion discs, black hole physics, methods: statistical, ISM: jets and outflows, X-rays: binaries
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