A Possible Signature of Connection between Blazars and Seyfert Galaxies

Details A Possible Signature of Connection between Blazars and Seyfert Galaxies A Possible Signature of Connection between Blazars and Seyfert Galaxies

Oct 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003pasj...55..947l&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.55, No.5, pp. 947-951

Astronomy and Astrophysics

Astronomy

Galaxies: Active, Galaxies: Bl Lacs, Galaxies: Evolution, Galaxies: Nuclei, Galaxies: Seyfert

Scientific paper

The accretion rates (dot{M}) and their correlation with cosmological redshifts for a sample of blazars and Seyfert galaxies are presented. The sample includes 77 blazars (28 FSRQs, 26 LBLs, and 23 HBLs) and 60 Seyfert galaxies, of which the extended spectral energy distribution information and redshifts are available. Within the framework of accreting black holes, the accretion rates for these sources were estimated based on their bolometric luminosities. The result shows that the accretion rates are significantly different for each subclass of the blazars and Seyfert galaxies. Their averages are, respectively, 50.2, 17.0, 1.0, 0.1Modot yr-1 for the FSRQs, LBLs, HBLs, and the Seyfert galaxies, exhibiting a well descending sequence of FSRQs-LBLs-HBLs-Seyfert galaxies. They are strongly correlated with the redshifts for both blazars and Seyfert galaxies. The linear correlation coefficients are 0.81 and 0.68 with a chance probab ility of p < 0.0001, respectively. A plot of dot{M} - z shows that the blazars and the Seyfert galaxies distribute in a distinguishable regions with a connection at z ˜ 0.7 and almost all the sources lie in a narrow region of z1.40 ≤ dot{M} ≤ 250 z1.40, illustrating a strong correlation between the two quantities for the whole sample. The regression line is dot{M} = (14.5 ± 1.2) z1.40±0.06 Modot yr-1 with a linear coefficient of 0.93 and a chance probability of p < 0.0001, suggesting a connection between blazars and Seyfert galaxies. This connection might imply that the two classes are on the same evolutionary sequence. Although the correlations of the data are formally solid, the conclusion may be affected by one source of considerable uncertainty at the data level, which is also discussed.

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