COSMOGONY AND COSMOLOGY

Author: PASCUAL RAMÍREZ SERGIO.
Year: 2003.
University: COMPLUTENSE DE MADRID.
Place of defense: FACULTAD DE CIENCIAS FÍSICAS.
Place of preparation: FACULTAD DE CC FÍSICAS.

Summary: The work dela thesis focuses on the search for emission-line galaxies with H algae to shift red z = 0.24 and z = 0.4. These movements towards the red line emission is in the longudes wave the 820m and 920m, where bands of atmospheric OH presents a local minimum. This allows you to use filters that focus on narrow wavelengths to select candidates for an excess emission in these feltros when compared caring filters wide. Based on the selected objects are contruye a sample is studied and the rate of formation of the universe such stellar travel rojo.La rate fromación stellar found is consistent with a strong increase between z = 0 z = 1,

Author: SÁNCHEZ BLÁZQUEZ PATRICIA.
Year: 2003.
University: COMPLUTENSE DE MADRID.
Place of defense: FACULTAD DE FÍSICAS.
Place of preparation: FACULTAD DE FÍSICAS.

Summary: One delos fundamental problems of modern Astronomy is knowing how and when they formed the galaxias.De primary importance for achieving this goal is to know what kind of people stellar albergan.En this thesis is a study of its spectra integrados.Debido to the enatrono in the galaxies they inhabit has been a decisive factor in the processes of formation and subsequent evolution of the same in this report are pueso special interest in studying the stellar populations in galxias in environments difente densidad.Aunque originally it was thought that galaxies of parimeros types were older systems that were formed when the universe was still young, and had evolved passively until today, recently tothe development of new and better telescopes are discovering that these systems have great morphological characteristics and quantity of cinematic and that many of them seem alberggar populations stellar relativamelnte youth. To lose estimate parameters that characterize the stellar populations makes use of models synthesis poblaciones.Uno of the key ingredients of these models are libraries estelares.En this work is conducted xonstrucción a new library stellar higher number and as to libraries used prior to the fecha.La inclusion of this new library synthesis models population has reduced machas of uncertainties that, so far affecting these models. Once improved tools, we performed far 21 features on the spectral central spectra of galaxies and also in taste over radio.Los results of this thesis suggests that, contrary to the classical view, of galaxies primary types in entronos low density have had a stellar formation extended in time, that explain its major properties if they have sufrifo different episiodos training estelar.Sin embargfo, this is not true when the study raliza on galaxies in the cluster dense Coma, where there is a population more homogeneous and consistent with the classic scene in formation of galaxies first galaxies inhabit influences, so decisive in the history of the stellar formation that have experimentado.Por other hand, through the study the gradients caracterésticas spectral, it has been shown that the galaxies situaadas in different environments were formed, most likely through mechanism diferentes.Así, while the observations of galaxies Coma suggest that these could be forming from collapse disipativo a cloud, or from mergers of gaseous systems (which have not yet become stars in this gas), the galaxies in estornos less dense have formed from mergers of systems, in which the proportion of mass stars respect mass gas increases with the mass of mismos.Estos is what the model predicts low formation of galaxies through hierarchical clustering.

Author: FERNANDEZ CEREZO SILVIA.
Year: 2004.
University: LA LAGUNA.
Place of defense: UNIVERSIDAD DE LA LAGUNA.
Place of preparation: INSTITUTO DE ASTROFISICA DE CANARIAS.

Summary: This thesis is devoted to the study of diffuse galactic emission and anisotropies of the cosmic microwave radiation through the observations of the experiment COSMOSOMAS. It also discusses these emissions in the WMAP maps published after the first year of operation of the satellite. We present maps COSMOSOMAS to 12.7, 14.7 and 16.3 GHz obtained from the clustered around 100 working days observing every frecuecia, These maps contain angular scales between 1Â º and 5Â eighth, and cover an area of 9000 degrees square is complete in ascension and 30Â º coverage in decline. The noise level of these maps is 63 micro-K beam to 12.7 and 14.7 GHz and 120 micro-K beam to 16.3. Analysis of the signal present in the diffuse galactic maps COSMOSOMAS and WMAP is done through the correlation of these observations with tracer maps of the different types of diffuse galactic emission. Positive correlations were found on maps of our experiment with maps of synchrotron emission, H alpha and galactic dust. It has also been detected signal in common among low-frequency maps and maps of WMAP synchrotron emission from the galactic dust. The correlation with existing maps emission dust is a new detection of what has been broadcast denominando anomalous (since our observation frequencies not expect any signal due to the well-known dust emission, emission vibrational). The intensity of the emission from anomalous increases frequencies observation WMAP those of COSMOSOMAS, the maximum emission detected in the channel with the highest frequency of COMOSOMAS with an intensity of about 17 micro K. That issue falls sharply with the galactic latitude. At correlar observations COSMOSOMAS with individual channels WMAP is a signal common to both experiments whose intensity falls gently with the frequency channel WMAP. The signal correlada with channels highest frequency of WMAP is of the order of 30 micro-K, power expected for the anisotropies of the RCM. The biggest intenisdad the signal correlada in channels of lowest frequency of WMAP is due to the presence of contamination galactic and extragalactic. The apliación of the art Multi-Detector Multi-Component Spectral Matching (MDMC) has led to the separation of components in maps COSMOSOMAS and WMAP. With this technique has been identified component of the anisotropies of the RCM, a component of noise common to the three channels of our experiment, which was perhaps home atmosphere, and a component that is a mixture of different types of galactic emission.

Author: BALAGUER NÚÑEZ M. DE LOS DOLORES.
Year: 2005.
University: BARCELONA.
Place of defense: FACULTAD DE FÍSICA.
Place of preparation: FACULTAD DE FÍSICA.

Summary: The thesis aims to improve the characterization of open clusters NGC 1807, NGC 1817, NGC 24548 (M 48) and NGC 2682 (M 67), as well as study their situation in the context of system galactic open clusters. For there have been catalogs full photometry and astrometry of the area of cumulus, lists of members in each cluster, have been studied their fundamental physical parameters (redness, metallicity, distance, age, mass, size, orbital parameters ..) its luminosity and mass functions, its most prominent stars (behind blue, red giants, binary ..), as well as the degree of segregation mass of each. Moreover these results were compared with the system's open galactic clusters studied more general properties such as the relationship of age, and metallicity distance. It also has been searching for holes in the main sequence data that have resulted in the characterization of a possible hollow unknown until this study.

Author: GENOVA SANTOS RICARDO TANAUSU.
Year: 2006.
University: LA LAGUNA.
Place of defense: UNIVERSIDAD DE LA LAGUNA.
Place of preparation: UNIVERSIDAD DE LA LAGUNA.

Summary: In this thesis was presented a study of the primary and secondary anisotropies Fund's Cosmic Microwave (FCM) in intermediate angular scales (between 2Â ° and 11 minutes of arc), primarily using observations interferometer Very Small Array (VSA). This instrument is located at the Observatorio del Teide and operates at a frequency of 33 GHz. The study of anisotropies primary FCM is now one of the tools most important from the point of view of the characterization of the cosmological model of the Universe. It also addresses the problem of the distribution of local baryons in the Universe, where roughly half the content bariónico estimate has not yet been detected. The hydrodynamic simulations of structure formation suggests that these baryons undetected structures could be found in large-scale, low-density and intermediate temperatures, around the regions with the highest concentration of matter. Emplemos effect Sunyaev-Zeldovich (SZ), one of the most important secondary anisotropies, to study the distribution of baryons in: i) scales of galaxy clusters, where this effect is well characterized; ii) scales superclusters of galaxies ( > 0.5 Â °), with the aim of finding signs of diffuse gas structures that could accommodate the missing baryons.