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Luminosities of Radio-Loud Active Galaxies
We investigate the host galaxy luminosities of three different samples of radio loud active nuclei at z<0.5 including BL Lac Objects (BLLs), Radio... -
Probing the Evolution of Massive Galaxies with the K20 Survey
The motivations and the status of the K20 survey are presented. The first results on the evolution of massive galaxies and the comparison with the... -
The Evolution of Galaxy Mass in Hierarchical Models
Advances in extragalactic astronomy have prompted the development of increasingly realistic models which aim to describe the formation and evolution... -
Studying the Dynamics of Star Forming and IR Luminous Galaxies with Infrared Spectroscopy
With the advent of efficient near-IR spectrometers on 10m-class telescopes, exploiting the new generation of low readout noise, large format... -
What Does the Local Black Hole Mass Distribution Tell Us About the Evolution of the Quasar Luminosity Function?
We present a robust method to derive the duty cycle of QSO activity based on the empirical QSO luminosity function and on the present-day linear... -
Spheroidal Galaxies/QSOs Connection
In view of the extensive evidence of a tight inter-relationship between spheroidal galaxies (and galactic bulges) and massive black holes hosted at... -
The Mass of Radio Galaxies from Low to High Redshift
Using a new radio sample, 6C* designed to find radio galaxies at z > 4 along with the complete 3CRR and 6CE sample we extend the radio galaxy K-z... -
Estimating the Mass of Local Disk Galaxies from the NIR Luminosity
The relation between the dynamical mass ( $\propto V_{max}^2 \times r_{opt}$... -
Clustering at High Redshift
The addition of deep near infrared images to the database provided by the HDF WFPC2 is essential to monitor the SEDs of the objects on a wide... -
Detection of CDM Substructure
The properties of multiple image gravitational lenses require a fractional surface mass density in satellites of f... -
Lens Galaxies vs. CDM
By directly probing mass distributions, gravitational lensing offers several new tests of the CDM paradigm. Lens statistics place upper limits on the... -
Galaxy-Galaxy Lensing in the FORS Deep Field
We demonstrate the presence of a galaxy-galaxy lensing signal of z=0.5-1.0 foreground galaxies by analyzing the distortion of z=2.5-4.5 background... -
The Mass Function of Field Galaxies at 0.4 < z < 1.2 as Derived from the MUNICS K-Selected Sample
We derive the number density evolution of massive field galaxies in the redshift range 0.4 < z < 1.2 using the K-band selected field galaxy sample... -
Nuclear Stellar Disks in Spiral Galaxies
We report the discovery of a nuclear stellar disk in 3 early-type spirals, namely NGC 1425, NGC 3898 and NGC 4698, revealed by WFPC2/F606W images out... -
Gas Minor-Axis Velocity Gradients in Early-Type Spiral Galaxies
We measured a remarkable gas velocity gradient along the minor axis of 5 early-type spiral galaxies. This phenomenon suggests the presence of a... -
The Evolution of Distant Cluster Spirals
Ground-based and HST observations indicate that the disk galaxy population in rich galaxy clusters has experienced remarkable evolution since z = 1.... -
Measuring Galaxy Disk Mass with the SparsePak Integral Field Unit on WIYN
We present first results from the commissioning data of the SparsePak Integral Field Unit on the WIYN telescope. SparsePak is a bundle of 82 fibers,... -
Constraining the Mass Assembly in Ellipticals from ERO Clustering
The redshift evolution of clustering is a powerful tool to constrain the models of galaxy assembly. In particular, the strong clustering of EROs, if... -
Evolution in the Linewidth-Magnitude Relation to z > 1 from the DEEP Groth Strip Survey
Galaxy kinematics are potentially a powerful tool to measure the evolution of Tully-Fisher-type relations and to see how properties of distant... -
First Evidence for an Extended Dark Halo in the Draco Dwarf Spheroidal
We present a new velocity data set in the Draco dwarf spheroidal, containing the velocities of 159 giant stars extending to large radii. We fit this...