2009/07/13 by Qingwen Wu, QingWen Wu, Minfeng Gu +2
Physics and Astronomy · #Accretion (finance) #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #Galaxy #QSOS #QUIET #Radio galaxy #Radio spectrum #Redshift #X-shaped radio galaxy #astro-ph.CO #astro-ph.HE
paper · pdf · doi:10.1007/s11433-010-0016-2
published as Sci. China G53:235-239,2010 · 5 pages, 4 figures, accepted by Science in China Series-G (BH issue), only PDF, which is relate to recent two papers arXiv:0905.3663(MNRAS, in press) and arXiv:0907.2234 (ApJL, in press)
arxiv created 2009/07/13 · openalex publication_date 2010/01/01 · arxiv updated 2014/11/20 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We estimate black hole masses and Eddington ratios for a sample of 81 young radio galaxies (42 CSS +39 GPS). We find that the average black hole (BH) mass of these young radio galaxies is <log Mbh>~8.3, which is less than that of radio loud QSOs and low redshift radio galaxies. The CSS/GPS sources have relatively high Eddington ratios, with an average value of <log Lbol/LEdd>=-0.75, which are similar to those of narrow line Seyfert 1 galaxies (NLS1s). This suggests that young radio galaxies may not only be in the early stages of their radio activity, but also in the early stage of their accretion activity. We find that the young radio galaxies as a class deviate systematically from Mbh-σrelation defined by nearby inactive galaxies, when using [O III] as a surrogate for stellar velocity dispersion, σ_* . We also find that the deviation of the [O III] line width is correlated with the Eddington ratio and sources with Lbol/LEdd~1 have the largest deviations, which are similar to those of radio quiet QSOs/NLS1s (radio jets is absent or weak). A similar result has been obtained for 9 linear radio Seyfert galaxies. On the basis of these results, we suggest that, in addition to the possible jet-gas interactions, accretion activities may also play an important role in shaping the kinematics of the narrow [O III] line in young radio galaxies and linear radio Seyferts.