A Generalized Lagrange Multiplier Method for Support Vector Regression with Imposed Symmetry

This thesis presents an approach to support vector regression that extends the classic Vapnik’s formulation. After recalling that the classic formulation contains a Lasso regularization structure in its dual form, we propose a generalized Lagrangian function with additional terms to include the Ridge regularization in the dual problem for the case with symmetry. By including both regularization methods, the resulting dual problem with the generalized Lagrangian comprises an elastic net regularization structure. Hence, as an immediate consequence, the classical formulation is a particular case of the current proposal. Finally, to demonstrate the capabilities of this approach, the document includes examples of predicting some benchmark problems

Kn 26, a New Quadrupolar Planetary Nebula

Once classified as an emission line source, the planetary nebula (PN) nature of the source Kn 26 has been only recently recognized in digital sky surveys. To investigate the spectral properties and spatio-kinematical structure of Kn 26, we have obtained high spatial-resolution optical and near-IR narrow-band images, high-dispersion long-slit echelle spectra, and intermediate-resolution spectroscopic observations. The new data reveal an hourglass morphology typical of bipolar PNe. A detailed analysis of its morphology and kinematics discloses the presence of a second pair of bipolar lobes, making Kn 26 a new member of the subclass of quadrupolar PNe. The time-lap between the ejection of the two pairs of bipolar lobes is much smaller than their dynamical ages, implying a rapid change of the preferential direction of the central engine. The chemical composition of Kn 26 is particularly unusual among PNe, with a low N/O ratio (as of type II PNe) and a high helium abundance (as of type I PNe), although not atypical among symbiotic stars. Such an anomalous chemical composition may have resulted from the curtail of the time in the Asymptotic Giant Branch by the evolution of the progenitor star through a common envelope phase.Comment: 9 pages, 5 figures, accepted for publication in A&

CRIRES-VLT high-resolution spectro-astrometry as a tool in the search of small structures at the cores of Planetary Nebulae

The onset of the asymmetry in planetary nebulae (PNe) occurs during the short transition between the end of the asymptotic giant branch (AGB) phase and the beginning of the PN phase. Sources in this transition phase are compact and emit intensely in infrared wavelengths, making high spatial resolution observations in the infrared mandatory to investigate the shaping process of PNe. Interferometric VLTI IR observations have revealed compelling evidence of disks at the cores of PNe, but the limited sensitivity, strong observational constraints, and limited spatial coverage place severe limits on the universal use of this technique. Inspired by the successful detection of proto-planetary disks using spectro-astrometric observations, we apply here for the first time this technique to search for sub-arcsecond structures in PNe. Our exploratory study using CRIRES (CRyogenic high-resolution Infra-Red Echelle Spectrograph) commissioning data of the proto-PN IRAS 17516-2525 and the young PN SwSt 1 has revealed small-sized structures after the spectro-astrometric analysis of the two sources. In IRAS 17516-2525, the spectro-astrometric signal has a size of only 12 mas, as detected in the Brackett-gamma line, whereas the structures found in SwSt 1 have sizes of 230 mas in the [Fe III] line and 130 mas in the Brackett-gamma line. The spectroscopic observations required to perform spectro-astrometry of sources in the transition towards the PN phase are less time consuming and much more sensitive than VLTI IR observations. The results presented here open a new window in the search of the small-sized collimating agents that shape the complex morphologies of extremely axisymmetric PNe.Comment: 6 pages, 4 figure

VISIR-VLT Images of the Water Maser Emitting Planetary Nebula K 3-35

K3-35 is an extremely young bipolar planetary nebula that contains a precessing bipolar jet and a small (radius 80 AU) water maser equatorial ring. We have obtained VISIR- VLT images of K 3-35 in the PAH1 ({\lambda}=8.6 {\mu}m), [S iv] ({\lambda}=10.6 {\mu}m), and SiC ({\lambda}=11.85 {\mu}m) filters to analize the mid-IR morphology and the temperature structure of its dust emission. The images show the innermost nebular regions undetected at optical wavelegths and the precessing bipolar jets. The temperature map shows variations in the temperature in the equatorial zone and in regions associated to its jets.Comment: 2 pages, 2 figures, 283 IAU Symp. Planetary Nebulae an Eye to the Futur

Disinfection Potential of the Catalytic Wet Peroxide Oxidation (CWPO) for inactivation of intestinal parasites Giardia lamblia and Cryptosporidium parvum

Introduction WHO (World Health Organization) has estimated that around 24 % of the diseases at a global scale are related to environmental factors like consumption of insecure drinking water. Recent laws have become more stringent about the permitted parameters of quality, including more careful surveillance on the presence of resistant forms of Giardia (cysts) and Cryptosporidium (oocysts) in water for human consumption. It has been pointed out that some particular physicochemical properties of their cysts/oocysts cell walls make them strongly resistant against conventional chlorine disinfection [1]. Moreover, complex mechanisms there implied are not still completely elucidated. Therefore, conventional disinfection by chlorine should be assisted or even replaced by novel, safer technologies like the advanced oxidation processes (AOPs). The CWPO is a very efficient, not expensive AOP [2] that could offer a very interesting performance for effective and safe inactivation of resistant pathogen agents like the cysts/oocysts of the intestinal parasites Giardia and Cryptosporidium, even under very mild conditions of ambient temperature and pressure (15 – 25 °C; < 1 atm). This work is devoted to explore the true potential of the CWPO technology in the inactivation of these couple of resistant forms of dangerous parasites

The triple-shell structure and collimated outflows of the planetary nebula NGC 6891

Narrow-band H$\alpha$ and [N {\sc ii}] images and high-dispersion spatially-resolved echelle spectroscopy of the planetary nebula NGC 6891 are presented. These observations show a great wealth of structures. The bright central nebula is surrounded by an attached shell and a detached outer halo. Both the inner and intermediate shells can be described as ellipsoids with similar major to minor axial ratios, but different spatial orientations. The kinematical ages of the intermediate shell and halo are 4,800 and 28,000 years, respectively. The inter-shell time lapse is in good agreement with the evolutionary inter-pulse time lapse. A highly collimated outflow is observed to protrude from the tips of the major axis of the inner nebula and impact on the outer edge of the intermediate shell. Kinematics and excitation of this outflow provide conclusive evidence that it is deflected during the interaction with the outer edge of the intermediate shell. At the same time, both the kinematics and the morphology of the intermediate shell appear to be affected by this interaction.Comment: To be published in MNRAS, 9 pages, 5 figure