Results 101 to 110 of about 160 (135)
Morphology of Seyfert Galaxies [PDF]
Astrophysics and Space Science, 2017 We probed the relation between properties of Seyfert nuclei and morphology of their host galaxies. We selected Seyfert galaxies from the Sloan Digital Sky Survey with redshifts less 0.2 identified by the Véron Catalog (13th). We used the "{\it{FracDev}}" parameter from SDSS galaxy fitting models to represent the bulge fractions of the Seyfert host ...
Chorng-Yuan Hwang
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Seyfert Galaxies And Their Environment
Symposium - International Astronomical Union, 1999The role played by environment on nuclear activity in galaxies is not clear and largely debated (see e.g. Barnes & Hernquist 1992, Kelm 1996). To overcome statistical uncertainties, environment properties of two large samples of Seyfert galaxies (Sy 1 and Sy 2 have been kept separated) have been computed and compared with equivalent size “normal ...
P. Focardi, B. Kelm, G.G.C. Palumbo
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A Spectropolarimetric Atlas of Seyfert 1 Galaxies [PDF]
Monthly Notices of the Royal Astronomical Society, 2002 We present optical spectropolarimetry of the nuclei of 36 Seyfert 1 galaxies, obtained with the William Herschel and the Anglo-Australian Telescopes from 1996 to 1999. In 20 of these, the optical emission from the active nucleus is intrinsically polarized.
J H Hough, D J Axon
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HNC and HCN in Seyfert Galaxies
EAS Publications Series, 2008What are the physical conditions in the nuclear region of Seyfert galaxies? Can we asses the predominant nuclear source of power starburst or AGN by using high density gas tracers? We have used SEST, JCMT, and IRAM 30 m telescopes to observe the J = 1 - 0, J = 3 - 2, and J = 4 - 3 transition lines of HNC and HCN in the Seyfert 2 galaxies NGC 1068 and ...
Perez-Beaupuits, J. P. +3 more
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Narrow-Line Seyfert 1 Galaxies and the Evolution of Galaxies and Active Galaxies [PDF]
Monthly Notices of the Royal Astronomical Society, 2000 Narrow Line Seyfert 1 galaxies (NLS1s) are intriguing due to their continuum as well as emission line properties. The observed peculiar properties of the NLS1s are believed to be due to accretion rate close to Eddington limit. As a consequence, for a given luminosity, NLS1s have smaller black hole (BH) masses compared to normal Seyfert galaxies.
Smita Mathur
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AIP Conference Proceedings, 1997
Observations with Compton Gamma Ray Observatory have provided key insights to the high energy emission mechanisms in Active Galactic Nuclei (AGN) and clearly separate them into a class of Blazars, with apparent non-thermal jet emissions often peaking in the EGRET energy band, and into the Seyfert class with emissions more closely related to the ...
W. Neil Johnson +5 more
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Observations with Compton Gamma Ray Observatory have provided key insights to the high energy emission mechanisms in Active Galactic Nuclei (AGN) and clearly separate them into a class of Blazars, with apparent non-thermal jet emissions often peaking in the EGRET energy band, and into the Seyfert class with emissions more closely related to the ...
W. Neil Johnson +5 more
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The environment of seyfert galaxies
Chinese Astronomy and Astrophysics, 1986Abstract We made a nearest neighbour analysis on the cluster galaxies in the CfA sample. We found that galaxies with nearest distances below 20 kpc show a clear excess of Seyfert nuclei (i.e., the incidence of Seyferts among such galaxies is about 3 times higher than the average).
null Chen Jian-sheng, null Zou Zhen-long
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Infrared Background from Seyfert Galaxies
Nature, 1970Kleinmann and Low1 and Low2 have recently reported measurements of the infrared spectrum of the Seyfert galaxy NGC 1068. The spectrum was found to be sharply peaked at a wavelength of ∼100 µm (with an uncertainty of a factor of two or three toward longer wavelengths), while the total infrared luminosity amounts to L∼2.5 × 1046 erg s−1 (for a Hubble ...
G, Setti, L, Woltjer
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Seyfert Galaxies in the Universe
1986Recent optical spectroscopy of Seyfert galaxies, particularly at Lick Observatory, is discussed. The frame of reference is the luminosity function of Seyfert galaxies, the incompleteness of available surveys, and how complete samples can be found by combining several different types of surveys.
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