BLACK HOLE MASSES AND HOST GALAXY EVOLUTION OF RADIO-LOUD ACTIVE GALACTIC NUCLEI
Author
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Woo, Jong-Hak
Author
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Urry, C. Megan
es_CL
Author
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van der Marel, Roeland P.
es_CL
Author
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Lira Teillery, Paulina
es_CL
Author
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Maza Sancho, José
es_CL
Admission date
dc.date.accessioned
2013-12-26T20:22:33Z
Available date
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2013-12-26T20:22:33Z
Publication date
dc.date.issued
2005-10-01
Cita de ítem
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The Astrophysical Journal, 631:762–772, 2005 October 1
en_US
Identifier
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https://repositorio.uchile.cl/handle/2250/125871
Abstract
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We report stellar velocity dispersion measurements for a sample of 28 active galactic nucleus (AGN) host
galaxies, including our previous work. Using the mass-dispersion (M.- ) and the fundamental plane relations, we
estimate the black hole mass for a sample of 66 BL Lac objects and investigate the role of black hole mass in the
energetics of BL Lac objects. The black hole mass range for different BL Lac spectral types is similar, 107 <
M < 4 ; 109. Neither X-ray nor radio luminosity correlates with black hole mass. Low-frequency–peaked BL Lac
objects have higher Eddington ratios on average, because of either more beaming or higher intrinsic power. For the
black hole mass range 3 ; 107 < M <109, the radio luminosity of BL Lac objects and flat-spectrum radio quasars
spans over 4 orders of magnitude,with BL Lac objects being low-powerAGNs.We also investigate the evolution of
host galaxies for 39 AGNs out to z 0:5 with measured stellar velocity dispersions. Comparing the mass-to-light
ratio evolution in the observed frame with population synthesis models, we find that single-burst star formation
models with zform ¼ 1:4þ0:9
0:2 are consistent with the observations. From our zform ¼ 1:4 model, we estimated the
intrinsic mass-to-light ratio evolution in the Cousins R band, log (M/L)/ z ¼ 0:502 0:08, consistent with
that of normal early-type galaxies.
en_US
Patrocinador
dc.description.sponsorship
This research is a part of the AGN Key Project of the Yale-
Calan collaboration and has been supported by Fundacion Andes.
Partial support was also provided by NASA grant AST 04-07295.