Low- and intermediate-mass stars (1--8 M&sun;) lose up to 80 % of their initial mass during the Asymptotic Giant Branch (AGB) phase. Heavy mass loss is the signature of the late AGB phase: at uncertain rates of 10-6 to 10-3 M&sun; yr-1, on timescales of ˜ 10^5--10^6 yr, it removes up to 7 M&sun; of stellar material. We have investigated the

This thesis investigates the abundance and properties of extremely red galaxies (EROs). Although the existence of such conspicuous galaxies has been known for some time, there are numerous open questions regarding their nature, formation, and evolution. One reason is the number of different colour criteria applied to select EROs. Hence, different

To assess the possible utility of machine learning for classifying subjects with and subjects without osteoarthritis using sodium magnetic resonance imaging data. Theory: support vector machine, k-nearest neighbors, naïve Bayes, discriminant analysis, linear regression, logistic regression, neural networks, decision tree, and tree bagging were

We present integral field spectroscopy (IFS) of the central region of 3C 120. We have modeled the nuclear and host galaxy three-dimensional spectra using techniques normally applied to imaging, decoupling both components and obtaining a residual data cube. Using this residual data cube, we detected the extended emission line region associated with

Climate diagnostic studies combine data from different sources (radiosoundes, satellites, meteorological masts, etc) and meteorological models to predict the climate conditions and evolution at a particular site or globally. Products from climate diagnosis are archived in long-term databases that may constitute a useful tool for site

The standard ΛCDM model predicts that the major merger rate of galaxy-size dark matter halos rises rapidly with redshift. The average number of close companions per galaxy, Nc, is often used to infer the galaxy merger rate; however, recent observational studies suggest that Nc evolves very little with redshift. Here we use a ``hybrid'' N-body