The black hole mass, Eddington ratio, and M_bh-σ_[O III] relation in young radio galaxies

Details The black hole mass, Eddington ratio, and M_bh-σ_[O III] relation in young radio galaxies The black hole mass, Eddington ratio, and M_bh-σ_[O III] relation in young radio galaxies

2009-05-22

arxiv.org/abs/0905.3663v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

Accepted for pubblication in MNRAS, 10 pages, 8 figures

Scientific paper

The BH masses and the Eddington ratios for a sample of 65 young radio galaxies [27 GPS and 38 CSS sources] are estimated by various methods. We find that the average BH mass of these young radio galaxies is =8.3, which is less than that of radio loud QSOs and low redshift radio galaxies(=9.0). The CSS/GPS sources have relatively high Eddington ratios with average ratio =-0.56, which are similar to those of narrow line Seyfert 1 galaxies (NLS1s). It suggests that the CSS/GPS sources may not only be in the early stage of radio activities, but also in the early stage of their accretion activities. We find that the young radio galaxies as a class deviate systematically from the M_bh-\sigma_* relation defined by nearby inactive galaxies, when using \sigma_[O III] as a surrogate for the stellar velocity dispersion \sigma_*. There is no significant correlation between the deviation of the [O III] emission line width, $\Delta\sigma$=\sigma_[O III]-\sigma_[pred], and the jet/accretion power, where \sigma_[pred] are calculated from the Tremaine et al. relation using the estimated BH masses. However, we find that the deviation $\Delta\sigma$ in young radio galaxies is well correlated with the Eddington ratio, and this correlation is found to be similar to that of radio quiet AGN (QSOs/NLS1s) where the radio jet is absent or weak. We suggest that the accretion activities may still play an important role in shaping the kinematics of [O III] narrow line in these young radio galaxies.

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