We analyze a sample of 32 galaxies for which a dynamical estimate of the mass of the hot stellar component, M bulge , is available. For each of these galaxies, we calculate the mass of the central black hole, M • , using the tight empirical correlation between M • and the bulge stellar velocity dispersion. The frequency function N [log(M • /M bulge)] is reasonably well described as a Gaussian w...

We analyze a sample of 32 galaxies for which a dynamical estimate of the mass of the hot stellar component, M bulge , is available. For each of these galaxies, we calculate the mass of the central black hole, M • , using the tight empirical correlation between M • and the bulge stellar velocity dispersion. The frequency function N [log(M • /M bulge)] is reasonably well described as a Gaussian w...

In this paper, we present three qualitatively different scenarios for bulge formation: a secular evolution model in which bulges form after disks and undergo several central starbursts, a primordial collapse model in which bulges and disks form simultaneously, and an early bulge formation model in which bulges form prior to disks. We normalize our models to the local z = 0 observations of de Jo...

We present results of broad band BVRI observations of a sample of galaxies with a low surface brightness (LSB) disk and a bulge. These galaxies are well described as exponential disks and exponential bulges with no preferred value for either scale length or central surface brightness. The median B band disk scale length is 12.6 kpc (H0 = 75 km s−1 Mpc−1) which is much larger than scale lengths ...

Massive black holes detected in the centers of many nearby galaxies are linearly correlated with the luminosity of the host bulge, the black hole mass being about 0.1% of the bulge mass. An even stronger relation exists between the BH mass (Mbh) and the stellar velocity dispersion in the host bulge. We show that massive BHs of AGNs (measured by reverberation mapping) and their bulge luminosity ...

We analyse IRAS and COBE DIRBE data at wavelengths between 2.2 and 240 µm of the central 500 pc of the Galaxy and derive the large-scale distribution of stars and interstellar matter in the Nuclear Bulge. Models of the Galactic Disk and Bulge are developed in order to correctly decompose the total surface brightness maps of the inner Galaxy and to apply proper extinction corrections. The Nuclea...

Velocity, chemical abundance and spatial distribution data for some 1500 K-and M-giants in the Galactic Bulge, which are presented in an accompanying paper (Ibata & Gilmore 1995), are analysed. We provide three levels of analysis: an almost model-independent determination of basic symmetry properties of the galactic bulge; a more detailed analysis based on conservative assumptions, which invest...