Catálogo de publicaciones - libros

One approach to studying the epoch of galaxy formation is to infer formation redshifts from the ages of galaxies at known redshifts. When observed with optical instruments, galaxies lying at redshifts of z ~ 1 reveal their restframe UV spectra, which contain some features that show promise for breaking age-metallicity degeneracies inherent in techniques used for estimating galaxy ages. Early-type galaxies around the z ~ 1 epoch are of additional interest because they lie only a few Gyrs after the probable peak when galaxy mergers occurred. The spectra of young galaxies, such as these merger products, with ages of 1–5 Gyr are much more distinguishable than those of older galaxies, which results in more accurate age estimates.

A semi-analytic approach to the relativistic transport equation with isotropic diffusion and consistent radiative losses is presented. It is based on the eigenvalue method first introduced in Kirk & Schneider [5]and Heavens & Drury [3]. We demonstrate the pitch-angle dependence of the cut-off in relativistic shocks.

We discuss the effects of outbursts from supermassive black holes (SMBH) in luminous galaxies on surrounding gaseous atmospheres with emphasis on the Chandra observations of M87. The Chandra observations of M87 show both a system of buoyant bubbles as well as weak shock waves. In addition, we compare SMBH outbursts in systems from early type galaxies to rich clusters

The propagation of electromagnetic signals of pulsars through the non-stationary gravitational field of the stellar globular clusters formed by an ensemble of arbitrarily distributed stars are discussed. The expression for the relativistic time delay of pulsars radiation in such fields are derived taking into account the negligible aberration corrections. The obtained results are considered in the application to the globular cluster NGC 104 (Tucanae 47) for the cases of the small and large impact parameters.

We report a numerical result of jet formation driven by magnetic field due to a current loop around a rapidly rotating black hole. Beside the current loop, there are magnetic flux tubes that bridge the region between the ergosphere and the rotating disk, which we call ‘magnetic bridges’. The numerical result shows that the magnetic bridges can not be stationary and expand explosively to form a jet when the black hole rotates apidly.

We present a sample of the 22 most X-ray luminous galaxy clusters based on the ROSAT Bright Survey citekau_schwope. As all clusters are medium redshift systems (0.1< <0.52 ) their lensing probability is very high. We found gravitational arc candidates in ~70% of the clusters. In particular we focus on a combined lensing/X-ray analysis of one of the sample clusters, Z3146, based on deep ground based wide-field (WFI@ESO2.2m, B, V and R band), archival WFPC2@HST (F606W) and XMM/Newton observations.

We use two models in order to deal with a rotating universe. The first one is a thin rotating spherical shell. When we introduce in this shell an Hydrogen atom we found that the gravitomagnetic field of this universe can split the energy levels of the atom in a way analogous to the Zeeman effect.

The second model is the Gödel universe. There we use the solution of the Dirac equation on an arbitrary spacetime to find the shifts on energy levels of Hydrogen atoms caused by the rotation of the universe.

In both cases the interaction energy is very small, so we have to study the effect of cosmic rotation on Hydrogen atoms in a rotating expanding universe.

A semi-analytic approach to the relativistic transport equation with isotropic diffusion and consistent radiative losses is presented. It is based on the eigenvalue method first introduced in Kirk & Schneider [5]and Heavens & Drury [3]. We demonstrate the pitch-angle dependence of the cut-off in relativistic shocks.

One approach to studying the epoch of galaxy formation is to infer formation redshifts from the ages of galaxies at known redshifts. When observed with optical instruments, galaxies lying at redshifts of z ~ 1 reveal their restframe UV spectra, which contain some features that show promise for breaking age-metallicity degeneracies inherent in techniques used for estimating galaxy ages. Early-type galaxies around the z ~ 1 epoch are of additional interest because they lie only a few Gyrs after the probable peak when galaxy mergers occurred. The spectra of young galaxies, such as these merger products, with ages of 1–5 Gyr are much more distinguishable than those of older galaxies, which results in more accurate age estimates.

We report on the status of our effort to constrain the nature of dark energy through the evolution of the cluster mass function. temperature profiles for 31 clusters from a local cluster sample are shown. The X-ray appearance of the proto supermassive binary black hole at the center of the cluster Abell 400 is described. Preliminary weak lensing results obtained with Megacam@MMT for a redshift $z=0.5$ cluster from a distant cluster sample are given