In Abstract geometrical computation for black hole computation (MCU ’04, LNCS 3354), the author provides a setting based on rational numbers, abstract geometrical computation, with super-Turing capability: any recursively enumerable set can be decided in finite time. To achieve this, a Zeno-like construction is used to provide an accumulation similar in effect to the black holes of the black ho...

Chalcogen bonds are noncovalent interactions and increasingly coming into focus for the design of complex structures in research areas such as crystal engineering, molecular recognition catalysis. Conceptionally, chalcogen can be considered interaction between one σ-hole Lewis base center. Herein, we analyze bidentate chelating ligands having two nucleophilic centers with single a chalcogenazol...

The near-infrared integral field spectrograph SINFONI at the ESO VLT opens a new window for the study of central supermassive black holes. With a near-IR spatial resolution similar to HST optical and the ability to penetrate dust it provides the possibility to explore the low-mass end of the M•-σ relation (σ < 120 km s−1) where so far very few black hole masses were measured with stellar dynami...

We derive improved versions of the relations between supermassive black hole mass (MBH) and host-galaxy bulge velocity dispersion (σ) and luminosity (L) (the M–σ and M–L relations), based on 49 MBH measurements and 19 upper limits. Particular attention is paid to recovery of the intrinsic scatter (ε0) in both relations. We find log(MBH/M ) = α + β log(σ/200 km s−1) with (α, β, ε0) = (8.12± 0.08...

In this article we consider the growth of seed black holes immersed in dark matter halos. We first investigate the adiabatic growth in various initial distribution functions (isothermal, power law, and NFW) and find the resulting density, radial velocity, and anisotropy profiles. In addition we estimate the growth rate for a given black hole mass in the corresponding adiabatically modified dark...

In order to examine the relationship between the black hole mass MBH and stellar velocity dispersion σ∗ in radio-loud active galactic nuclei (AGNs), we study two effects which may cause the uncertainty of black hole mass estimates for radio-loud AGNs: the relativistic beaming effect on the observed optical continuum radiation and the orientation effect on broad emission line width. After correc...

Black hole masses in active galactic nuclei (AGN) are difficult to measure using conventional dynamical methods, but can be determined using the technique of reverberation mapping. However, it is important to verify that the results of these different methods are equivalent. This can be done indirectly, using scaling relations between the black hole and the host galaxy spheroid. For this purpos...

To examine the relationship between black hole mass and host galaxy velocity dispersion for low black hole masses, we have measured the velocity dispersions of 15 Seyfert 1 galaxies from the catalog of Greene & Ho (2004). These Seyferts were selected from the Sloan Digital Sky Survey to have estimated black hole masses below 106 M⊙. The data are consistent with a straightforward downward extrap...

We derive and discuss black–hole solutions to the gravitating O(3) σ model in (2+1) dimensions. Three different kinds of static black holes are found. One of these resembles the static BTZ black hole, another is completely free of singularities, and the last type has the same Penrose diagram as the (3+1)–dimensional Schwarzschild black hole. We also construct static and dynamical multi–black ho...

Using data of nearby galaxies from the Sloan Digital Sky Survey we investigate whether stellar mass (Mstar), central velocity dispersion (σ ), surface mass density (Σ), or the Sérsic n parameter is best correlated with a galaxy’s rest-frame color. Specifically, we determine how the mean color of galaxies varies with one parameter when another is fixed. When Mstar is fixed we see that strong tre...