XIE Zhao-hua, CHEN Luo-en, HAO Jian-ming, DU Lei-ming, ZHANG Xiong. Blazar Black Hole Masses[J]. Astronomical Techniques and Instruments, 2007, 4(2): 113-120.
Citation: XIE Zhao-hua, CHEN Luo-en, HAO Jian-ming, DU Lei-ming, ZHANG Xiong. Blazar Black Hole Masses[J]. Astronomical Techniques and Instruments, 2007, 4(2): 113-120.

Blazar Black Hole Masses

  • Black hole mass, along with the ratio of the accretionrate to the Eddington accretion rate, is a fundamental parameter of active galactic nuclei (AGNs).Using Xie's method of the black mass estimate, we developed our sample and estimated the black hole masses represented by MH for 21 blazars.We compare 21cases for each of which the relevant black hole mass has been also estimated by the MBH-σ correlation method, which is represented by Mσ.And we find that (1)MH are systematically lower thanMσ, but the differences between Mσ and MH are very small for most of the sources;(2)there is a significant correlation between Mσ and MH, the correlation coefficient r=0.823 with chance probability p~1.0×10-4.Based on these properties mentioned above and the standard model of AGNs, we prove that the nature of the systematical difference between Mσ and MH is that Mσ represents the mass in broad emission line region (r≤rb), while MH represents the mass in the continual emission region (r≤ra and ra rb)which is near the innermost stable orbit around the black hole.That is, Mσwould be overestimated.From Mσ, we calculate the central black hole mass again, which is indicated by MH*, and find that MH* is almost equal to the correspondent MH.
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