1. Investigating the relation of corona and disk from a blue AGN sample Liu, Jieying Yunnan Astronomical Observatory, CAS 第三届黑洞天体物理前沿问题年度研讨会 (2008),SHAO ， 26-28 April,2008

2. Using the observational data to investigate the accretion physics in RQ AGN, and constrain on accretion model. We also compare it with RL AGN in order to study underlying physics in accretion model. Motivation

3.  1) disk-corona model in AGN In luminous AGN and quasars,their SED indicates coexistence of hot gas and cool gas. The UV/optical emission arises from geometrically thin and optically thick cold disk (Shakura&Sunyeav,1973,A&A). The soft photons from the disk collide with the hot electrons in corona, emitting in X- ray( Liu,B.F.et al.2002,ApJL). 2) X-ray emission The dependence of X-ray emission on black hole mass and accretion rate can be different according to different accretion models (Narayan& Yi,1994;Merloni &Fabian 2002;Merloni et al.2003;Wang,J.M. et al,2004; Brandon et al.astro-ph/0801.2383v1) Introduction

4. RL: 18 RQ: 240 Radio loudness: Sample Total: 258 blue AGNs (free of dust extinction, the continuum Slope ≥ 1.5 ( f λ ∝ λ ^ (-α λ )), λ ranges from 4030-5600 ), redshift z ≤ 0.35,including Seyfert 1 galaxies and QSOs, objects covered by FIRST (gives f_20cm value),and have f_x(0.1-2.4 keV) （ Dong xiaobo et al. 2008,MRAS,383,581D) m: I band magnitude; t = -2.5log(F_20cm/3631 Jy) R i =log(f_20cm/f_iband)=0.4(m-t) ( et al.2002,AJ,128 )

5. Data analysis Black hole mass: Bolometric luminosity : ( Vestergaard & Peterson 2006,ApJ,641) (Kaspi et al 2000,ApJ,533; Elvis,M. et al 1994,ApJS,95) Eddingtong ratio: λ=L_bol/L_edd

6. X-ray luminosity: match with ROSAT bright and faint SRC Catalogue database Assuming: f_x(2keV)f_x(0.1-2.4 keV) f_x( 2-100 keV) For X-ray of 0.1-2.4 keV : the slope is different,the median is 1.73(phton index is 2.73) For hard X-ray(2-100 keV) : slope = 0.9(Reeves&Turner 2000,MNRAS)

7. Statistic result Z < 0.35,low redshift 10^6.5 < M_BH < 10^10

8.  The Eddington ratio ranges from 10^-2.5 to1.0,Most of them have strong disk radiation.

9. Spearman’s rank coefficient ρ= - 0.171 ， p=0.008 Assuming that the hard X-ray comes from corona, the correlation represents that the corona relative to disk becomes weaker as the Eddington ratio increases. Actually, the X-ray becomes softer as the increase of the accretion （ Lu&Yu,1999,ApJL). P is the two-sided significance of its deviation from zero,less than 0.05 means a significant correlation

10.  ρ= 0.002  P=0.969 There is no correlation between log(L_x/L_bol) and log( M_BH), implying that the accretion physics for AGN is similar in a large range of black hole mass. This could be extrapolated to BHXB.

11.  For RL AGNs, there is no significant correlation between log(L_x/L_bol) and Eddington ratio, it is different from RQ. This may be because the hard X-ray in RL AGNs is affected by jet.  There is also no correlation between log(L_x/L_bol) and the mass of BH. ρ = - 0.313 ， P=0.206 ρ= 0.281 ， P=0.259

12. Comparing with X-ray of 0.1-2.4 keV  The correlation is different from the hard X-ray, maybe the disk contributes a significant fraction on X-ray(0.1-2.4 keV). ρ= - 0.245 P = 0.0001 ρ= 0.139 P=0.031

13. 1. Both radio-loud and radio-quiet AGNs, logL_x/L_bol （ hard X-ray) is no correlate with log(M_BH). This implying that the accretion physics for AGN is similar in a large range of black hole mass. This could be extrapolated to BHXB. 2. logL_x/L_bol decreases with the increase of log(L_bol/L_Edd) for RQ AGNs. It is different with RL AGNs. 3. Different from the hard X-ray,the X-ray of 0.1- 2.4 keV may be connected with the disk radiation. Conclusion and discussion

14. Thank you ！