NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-05-24 T10:07:59 PDT
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For refcode 2011ApJS..195...23M:
Retrieve 45 NED objects in this reference.
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2011ApJS..195...23M Comparison of Millimeter-wave and X-Ray Emission in Seyfert Galaxies Monje, R. R.; Blain, A. W.; Phillips, T. G. Abstract. We compare the emission at multiple wavelengths of an extended Seyfert galaxy sample, including both types of Seyfert nuclei. We use the Caltech Submillimeter Observatory to observe the CO J = 2-1 transition line in a sample of 45 Seyfert galaxies and detect 35 of them. The galaxies are selected by their joint soft X-ray (0.1-2.4 keV) and far-infrared ({lambda} = 60-100 micron) emission from the ROSAT/IRAS sample. Since the CO line widths (W_CO_) reflect the orbital motion in the gravitational potential of the host galaxy, we study how the kinematics are affected by the central massive black hole (BH), using the X-ray luminosity. A significant correlation is found between the CO line width and hard (0.3-8 keV from Chandra and XMM-Newton) X-ray luminosity for both types of Seyfert nuclei. Assuming an Eddington accretion to estimate the BH mass (M_BH_) from the X-ray luminosity, the W_CO_-L_ X_ relation establishes a direct connection between the kinematics of the molecular gas of the host galaxy and the nuclear activity, and corroborates the previous studies that show that the CO is a good surrogate for the bulge mass. We also find a tight correlation between the (soft and hard) X-ray and the CO luminosities for both Seyfert types. These results indicate a direct relation between the molecular gas (i.e., star formation activity) of the host galaxy and the nuclear activity. To establish a clear causal connection between molecular gas and the fueling of nuclear activity, high-resolution maps (<100 pc) of the CO emission of our sample will be required and provided in a forthcoming Atacama Large Millimeter Array observation. Key words: galaxies: active, galaxies: ISM, galaxies: nuclei, galaxies: Seyfert
Retrieve 45 NED objects in this reference.
Please click here for ADS abstract

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