OPTICAL MONITORING OF THE BROAD-LINE RADIO GALAXY 3C 390.3*

摘要: We have undertaken a new ground-based monitoring campaign on the broad-line radio galaxy 3C?390.3 to improve measurement of size broad emission-line region and estimate black hole mass. Optical spectra g-band images were observed in late 2005 for three months using 2.4?m telescope at MDM Observatory. Integrated flux variations measured hydrogen Balmer lines H?, helium line He II?4686, as well fluxes optical active galactic nucleus (AGN) continuum ? =?5100 ?. The AGN vary simultaneously within uncertainties, ?cent = (0.2 1.1)?days. find that are delayed with respect variable by ?(H?) 56.3+2.4 6.6?days, 44.3+3.0 3.3?days, 58.1+4.3 6.1?days, ?(He II?4686) 22.3+6.5 3.8?days. blue red peaks double-peaked profiles, outer profile wings, ?3 days. This provides strong support gravitationally bound orbital motion dominant part line-emitting gas. Combining time delay emission H? separation profiles their rms spectra, we determine M vir bh 1.77+0.29 0.31 108 ?line 2.60+0.23 central 3C?390.3, respectively. Using inclination angle which is from superluminal detected range, accretion disk models fit X-ray observations, mass amounts 0.86+0.19 0.18 109 (peak separation) 1.26+0.21 0.16 (?line), result consistent masses indicated simple describe derived stellar dynamics radius-luminosity relation. Thus, radio-loud low Eddington ratio, L edd/L bol 0.02, follows same relation radio-quiet AGNs.