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For refcode 2012MNRAS.423.3118T:
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Copyright by Royal Astronomical Society. 2012MNRAS.423.3118T On the link between central black holes, bar dynamics and dark matter haloes in spiral galaxies Treuthardt, Patrick; Seigar, Marc S.; Sierra, Amber D.; Al-Baidhany, Ismaeel; Salo, Heikki; Kennefick, Daniel; Kennefick, Julia; Lacy, Claud H. S. Abstract. The discovery of a relationship between supermassive black hole (SMBH) mass and spiral arm pitch angle (P) is evidence that SMBHs are tied to the overall secular evolution of a galaxy. The discovery of SMBHs in late-type galaxies with little or no bulge suggests that an underlying correlation between the dark matter halo concentration and SMBH mass (M_BH_) exists, rather than between the bulge mass and M_BH_. In this paper we measure P using a two-dimensional fast Fourier transform and estimate the bar pattern speeds of 40 barred spiral galaxies from the Carnegie-Irvine Galaxy Survey. The pattern speeds were derived by estimating the gravitational potentials of our galaxies from K_s_-band images and using them to produce dynamical simulation models. The pattern speeds allow us to identify those galaxies with low central dark halo densities, or fast rotating bars, while P provides an estimate of M_BH_. We find that a wide range of M_BH_ exists in galaxies with low central dark matter halo densities, which appears to support other theoretical results. We also find that galaxies with low central dark halo densities appear to follow more predictable trends in P versus de Vaucouleurs morphological type (T) and bar strength versus T than barred galaxies in general. The empirical relationship between M_BH_ and total gravitational mass of a galaxy (M_tot_) allows us to predict the minimum M_tot_ that will be observationally measured of our fast bar galaxies. These predictions will be investigated in a subsequent paper. Key words: galaxies: fundamental parameters, galaxies: haloes, galaxies: kinematics and dynamics, galaxies: spiral, galaxies: structure
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