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Introduction L’évolution géopolitique des dernières décennies (après la chute du mur de Berlin en 1989) a initié un processus de réorientation du centre de gravité géopolitique vers le sud et l’est, en même temps que de nouveaux pays menaient un type de croissance propre à la mondialisation. Le Brésil a joué un rôle important dans ce processus, ainsi que l’Afrique du Sud à la limite orientale du bassin de l’Atlantique Sud. Dans le même temps, le Brésil a projeté ses droits juridictionnels sur...

Objective: Polypharmacy and overprescription of off-label medications are common in patients with borderline personality disorder (BPD). The aim of the present naturalistic study was to explore whether the skills training module of dialectical-behavioural therapy (DBT) can reduce polypharmacy in these patients in routine clinical practice. Methods: Retrospective, observational study of 377 patients with a primary diagnosis of BPD consecutively admitted to the BPD outpatient unit from 2010 through 2020. All patients were invited to participate in the DBT skills training module (DBT-ST). DBT-ST participants (n = 182) were compared with a control group who did not participate in DBT-ST (n = 195). Pre-post intervention changes in medication load and use of antidepressants, benzodiazepines, mood stabilizers, and antipsychotics were evaluated. Results: At baseline, most patients (84.4%) were taking at least one medication and 46.9% were on polypharmacy. Compared to controls, patients in the DBT-ST group presented a significant reduction in the number of medications (2.67–1.95 vs. 2.16–2.19; p < 0.001), medication load (4.25–3.05 vs. 3.45–3.48; p < 0.001), use of benzodiazepines (54.4%–27.5% vs. 40%–40.5%; p < 0.001), mood stabilizers (43.4%–33% vs. 36.4%–39.5%; p < 0.001), and antipsychotics (36.3%–29.1% vs. 34.4%–36.9%; p < 0.001). Conclusions: These findings suggest that patients with BPD can benefit from the DBT-ST module, which may reduce the medication load, particularly of sedatives. The results suggest that DBT-ST may be useful to treat overmedication in patients with BPD and could help to promote “deprescription” in clinical practice. This study was supported by Centro de Investigación Biomédica en Red de Salud Mental (CIBERSAM). The authors would like to thank Bradley Londres for professional English language editing.

Soziale Dienste zur Unterstützung von Menschen mit Behinderungen haben sich in den letzten Jahren dynamisch entwickelt und unterliegen auch aktuell einem erheblichen Veränderungsdruck. Die Forschungsarbeiten, die in diesem Band versammelt sind, haben die Entwicklung hin zu einer inklusionsorientierten Unterstützung in zahlreichen Projekten auf unterschiedlichen Ebenen aktiv begleitet., Social services to support persons with disabilities have developed dynamically in recent years and are currently subject to considerable pressure to change. The research work collected in this volume has actively accompanied the development towards inclusion-oriented support in numerous projects at different levels.

We present the third and final data release of the Large Early Galaxy Astrophysics Census (LEGA-C), an ESO/VLT public spectroscopic survey targeting $0.6 < z < 1.0$, Ks-selected galaxies. The data release contains 3528 spectra with measured stellar velocity dispersions and stellar population properties, a 25-fold increase in sample size compared to previous work. This $K_s$-selected sample probes the galaxy population down to $\sim0.3 L^*$, for all colors and morphological types. Along with the spectra we publish a value-added catalog with stellar and ionized gas velocity dispersions, stellar absorption line indices, emission line fluxes and equivalent widths, complemented with structural parameters measured from HST/ACS imaging. With its combination of high precision and large sample size, LEGA-C provides a new benchmark for galaxy evolution studies., Accepted for publication in ApJS. Data available at http://archive.eso.org/cms/eso-archive-news/Third-and-final-release-of-the-Large-Early-Galaxy-Census-LEGA-C-Spectroscopic-Public-Survey-published.html or https://users.ugent.be/\string~avdrwel/research.html\#legac

Resumen tomado de la publicación Mindfulness en el trastorno límite de la personalidad: el descentramiento media la efectividad del entrenamiento. Antecedentes: el entrenamiento de habilidades en Mindfulness es un componente central en la terapia dialéctica conductual para el tratamiento del trastorno límite de la personalidad (TLP). El objetivo del estudio fue comparar la efectividad del entrenamiento de habilidades DBT basado en mindfulness (DBT-M) con el entrenamiento de habilidades DBT basado en la efectividad interpersonal (DBT-IE), en reducir síntomas TLP. También evaluamos el mecanismo de acción específico de estas terapias a través de dos mediadores propuestos: descentramiento y desregulación emocional. Método: 102 participantes diagnosticados con TLP fueron incluidos en el estudio. Se realizaron Anova de medidas repetidas y análisis de mediación múltiple. Resultados: DBT-M fue más efectivo que DBT-IE en reducir síntomas TLP, aunque ambas intervenciones fueron eficaces para reducir la desregulación emocional. Identificamos un modelo de mediación en serie en el que DBT-M redujo síntomas TLP al aumentar la capacidad de descentramiento, lo que a su vez redujo la desregulación emocional. Este efecto de mediación mostró que los cambios en el descentramiento precedieron a las mejoras en la desregulación emocional. Conclusiones: estos hallazgos destacan el rol del descentramiento como un mecanismo de acción primario en DBT-M y sugiere que esta habilidad es un componente principal para el tratamiento del TLP. ESP

O objetivo deste artigo é analisar em que medida a governança da bacia Sul Atlântica leva à construção de uma comunidade transatlântica no Hemisfério Sul. Também visa compreender como a configuração de estruturas institucionais interferem nesse sistema e se configuram como frágeis laços político-culturais e econômicos transatlânticos. Embora no Atlântico Sul – diferentemente da Bacia do Norte – não tenha sido construída uma poderosa rede de interesses comuns, a expansão jurisdicional exige que Estados Costeiros adotem políticas marítimas proporcionais à magnitude da responsabilidade territorial adquirida, a qual a sub-bacia americana (especificamente Brasil e Argentina) propugna por uma posição de dominância ao sul do paralelo zero.

Background Ayahuasca is a plant tea containing the psychedelic 5-HT2A agonist N,N-dimethyltryptamine and harmala monoamine-oxidase inhibitors. Acute administration leads to neurophysiological modifications in brain regions of the default mode network, purportedly through a glutamatergic mechanism. Post-acutely, ayahuasca potentiates mindfulness capacities in volunteers and induces rapid and sustained antidepressant effects in treatment-resistant patients. However, the mechanisms underlying these fast and maintained effects are poorly understood. Here, we investigated in an open-label uncontrolled study in 16 healthy volunteers ayahuasca-induced post-acute neurometabolic and connectivity modifications and their association with mindfulness measures. Methods Using 1H-magnetic resonance spectroscopy and functional connectivity, we compared baseline and post-acute neurometabolites and seed-to-voxel connectivity in the posterior and anterior cingulate cortex after a single ayahuasca dose. Results Magnetic resonance spectroscopy showed post-acute reductions in glutamate+glutamine, creatine, and N-acetylaspartate+N-acetylaspartylglutamate in the posterior cingulate cortex. Connectivity was increased between the posterior cingulate cortex and the anterior cingulate cortex, and between the anterior cingulate cortex and limbic structures in the right medial temporal lobe. Glutamate+glutamine reductions correlated with increases in the “nonjudging” subscale of the Five Facets Mindfulness Questionnaire. Increased anterior cingulate cortex-medial temporal lobe connectivity correlated with increased scores on the self-compassion questionnaire. Post-acute neural changes predicted sustained elevations in nonjudging 2 months later. Conclusions These results support the involvement of glutamate neurotransmission in the effects of psychedelics in humans. They further suggest that neurometabolic changes in the posterior cingulate cortex, a key region within the default mode network, and increased connectivity between the anterior cingulate cortex and medial temporal lobe structures involved in emotion and memory potentially underlie the post-acute psychological effects of ayahuasca.

Patients with heart failure (HF) undergoing cardiac resynchronization therapy (CRT) who exhibit above-expected improvement are known as super-responders. We assessed the rate of super-responders in a population with left bundle branch block (LBBB) > 150 ms in the absence of scar tissue in the left ventricular posterolateral wall as well as prognostic variables. In this prospective observational cohort study (n=20) an electrocardiogram (ECG) was performed pre- and post-CRT. The classic and Strauss LBBB criteria were adopted (> 150 ms). The percent (%) reduction of the QRS was calculated after implantation. All patients responded to the Minnesota Living with Heart Failure questionnaire and underwent an echocardiogram to measure left ventricular ejection function (LVEF), left atrium (LA) diameter, left ventricular end-systolic volume (LVEDV), left ventricular end-diastolic volume (LVESV), and left ventricular end-diastolic diameter (LVEDD) pre- and 6 months post-CRT. Cardiac magnetic resonance imaging (MRI) measured the presence of scar tissue in the posterolateral LV wall and the total scar burden (% LV mass). Fisher’s exact test and the Mann-Whitney test were performed to evaluate possible prognostic variables. The mean age was 58.20±8.79 years old, 60% female, with a mean LVEF of 28.15±5.10%, ECG with LBBB mean QRS of 162.15±7.86 ms, LBBB > 150 ms with Strauss standard in 90% of cases, and 90% with non-ischemic cardiomyopathy. Twelve cases (60%) of super-responders (reduction > 30% LVESV after 6 months) were observed. Super-responders did not present a difference in response in sex (12 vs 8 P=0.67), age (58.67 vs 57.7 P=087), Minnesota quality of life (55.50 vs 67.70 P=0.2), % initial QRS reduction (21.16 vs 18.69 P=0.21), LVEF (29.25 vs 26.5 P=0.38), LVEDD (66.33 vs 67.67 P=0.83), LVEDV (211.16 vs 228.53 P=0.75), LVESV (145.83 vs 167.00 P=0.75), or LA diameter (41.58 vs 43.63 P=0.45). The presence of LBBB > 150 ms, using the Strauss standard (90%) and the absence of scar in the posterolateral wall may account for these positive results. Super-responders benefit the most from CRT, and the results of this study can contribute to a better selection of CRT candidates.

In the original publication of this article [1] the funding acknowledgement for grant “PI13/00134, ERDF Funds” was missing.

Using high resolution spectra from the VLT LEGA-C program, we reconstruct the star formation histories (SFHs) of 607 galaxies at redshifts $z = 0.6-1.0$ and stellar masses $\gtrsim10^{10}$M$_{\odot}$ using a custom full spectrum fitting algorithm that incorporates the emcee and FSPS packages. We show that the mass-weighted age of a galaxy correlates strongly with stellar velocity dispersion ($��_*$) and ongoing star-formation (SF) activity, with the stellar content in higher-$��_*$ galaxies having formed earlier and faster. The SFHs of quiescent galaxies are generally consistent with passive evolution since their main SF epoch, but a minority show clear evidence of a rejuvenation event in their recent past. The mean age of stars in galaxies that are star-forming is generally significantly younger, with SF peaking after $z100$Myrs. This indicates that $z>2$ progenitors of $z\sim1$ star-forming galaxies are generally far less massive. Finally, despite considerable variance in the individual SFHs, we show that the current SF activity of massive galaxies ($>$L$_*$) at $z\sim1$ correlates with SF levels at least $3$Gyrs prior: SFHs retain `memory' on a large fraction of the Hubble time. Our results illustrate a novel approach to resolve the formation phase of galaxies, and in identifying their individual evolutionary paths, connects progenitors and descendants across cosmic time. This is uniquely enabled by the high-quality continuum spectroscopy provided by the LEGA-C survey., 18 pages, 9 figures, accepted by ApJ

Background: Chagas disease continues to be a serious public health problem, and accounts for 25-30% of the indications for cardiac stimulation in Brazil. Objective: To assess clinical and epidemiological characteristics of patients with Chagas disease, younger than 18 years, who had undergone pacemaker implantation in Brazil between 1994 and 2011, and its temporal trend. Methods: This was a cross-sectional analysis of data from the Brazilian Pacemaker Registry database. The following variables were analyzed: year when pacemaker was implanted, location, age, sex, ethnic group, functional class and the main electrocardiographic findings at baseline. Results: In a total of 183,123 implants performed between 1994 and 2011, 214 implants of cardiac stimulation device in Chagas disease patients aged younger than 18 years were identified. Mean age at implantation was 5.6 ± 6.2 years. Second- and third-degree atrioventricular blocks corresponded to 71% of indications for pacemaker implantation. Fifty-six percent of the procedures were performed in the southeast region. Regarding the total number of pacemaker implants per year, there was a remarkable increase in the implants for all causes. However, time series analysis of the implants in Chagas disease patients younger than 18 years revealed a significant reduction in the annual number of implants. Conclusion: There has been an important reduction in the number of pacemaker implantations among children and adolescents with Chagas disease, suggesting a reduction in the vertical transmission of the parasite. Resumo Fundamento: A doença de Chagas mantém-se como sério problema de saúde pública e tem sido responsável por aproximadamente 25% a 30% das indicações de estimulação cardíaca no Brasil. Objetivo: Estudar as características clínicas e epidemiológicas dos pacientes menores de 18 anos portadores de doença de Chagas submetidos a implante de marca-passo no território brasileiro entre 1994 e 2011, e sua tendência temporal. Métodos: Trata-se de um estudo retrospectivo que utilizou informações coletadas pelo Registro Brasileiro de Marca-passo. As variáveis analisadas foram: ano do implante, localidade, idade, sexo, grupo étnico dos pacientes; classificação funcional e os principais achados eletrocardiográficos de base. Resultados: Em um total de 183 123 implantes realizados entre 1994 e 2011, foram identificados 214 implantes de dispositivos de estimulação cardíaca em portadores de doença de Chagas com idade inferior a 18 anos. A média de idade no momento do implante foi de 5,6 ± 6,2 anos. Bloqueios atrioventriculares de 2º e 3º graus foram responsáveis por 71% das indicações. Dos procedimentos, 55,6% foram realizados na região sudeste. Em relação ao total de implantes de marca-passo por ano, observamos um aumento importante e significante de implante por todas as causas. Entretanto, quando avaliamos a série temporal de implantes em pacientes com doença de Chagas menores que 18 anos, observamos uma redução expressiva e significativa no número anual de implantes. Conclusão: Observa-se uma redução importante do número de implantes de marca-passo em crianças e adolescente chagásicos, o que sugere uma redução da transmissão vertical do parasita.

Las ciudades medias presentan ventajas frente a las grandes urbes y, por ello, deberían desempeñar funciones esenciales para el equilibrio territorial. Sin embargo, en los últimos tiempos, las Administraciones Públicas han destinado más inversiones a las grandes metrópolis, provocando una concentración demográfica, económica, de infraestructuras y equipamientos en éstas, con la consiguiente pérdida del protagonismo que las ciudades medias tenían décadas atrás. En el presente artículo se establecen tipologías de ciudades medias andaluzas en función de su localización para evaluar su evolución en los últimos tiempos. Mid-size towns and cities have certain advantages over large cities and ought to play essential roles in spatial balance. However, in recent times the Public Administration has allocated more investments to large metropolises, leading to demographic, economic and infrastructural and equipment concentration in these, and mid-size towns and cities consequently relinquishing the leadership that they used to have several decades ago. This article discusses some of the main types of Andalusian mid-size towns and cities on the basis of their location and the different ways that they have developed in recent times.

Background Impulsivity is considered a core characteristic of borderline personality disorder (BPD). Previous research on the effects of mindfulness training (MT) has shown that it might modify impulsivity-related aspects of BPD. Therefore, the aim of this study was to investigate the impact of MT on various facets of impulsivity in BPD patients. Methods Subjects with BPD diagnosis (n = 64) were randomly assigned to 10 weeks of MT (n = 32) or interpersonal effectiveness skills training (IE; n = 32). All participants were assessed pre- and post-intervention with a self-reported measure of impulsivity and five behavioral neuropsychological tasks to evaluate response inhibition, tolerance for delay rewards, and time perception. Results An interaction effect of time × group was only observed for some of the behavioral paradigms used. Participants in the MT group improved their ability to delay gratification and showed changes in time perception, consistent with a decrease in impulsivity. No differences were observed between treatments in terms of trait impulsivity and response inhibition. Conclusions Mindfulness training might improve some aspects of impulsivity but not others. Further study is warranted to better determine the effects of mindfulness training on the components of impulsivity. Trial registration ClinicalTrials.gov Identifier: NCT02397031. Electronic supplementary material The online version of this article (doi:10.1186/s40479-015-0035-8) contains supplementary material, which is available to authorized users.

The Spitzer Survey of Stellar Structure in Galaxies is a volume, magnitude, and size-limited survey of 2352 nearby galaxies with deep imaging at 3.6 and 4.5 μm. In this paper, we describe our surface photometry pipeline and showcase the associated data products that we have released to the community. We also identify the physical mechanisms leading to different levels of central stellar mass concentration for galaxies with the same total stellar mass. Finally, we derive the local stellar mass–size relation at 3.6 μm for galaxies of different morphologies. Our radial profiles reach stellar mass surface densities below ~1 M⊙ pc^(-2). Given the negligible impact of dust and the almost constant mass-to-light ratio at these wavelengths, these profiles constitute an accurate inventory of the radial distribution of stellar mass in nearby galaxies. From these profiles we have also derived global properties such as asymptotic magnitudes (and the corresponding stellar masses), isophotal sizes and shapes, and concentration indices. These and other data products from our various pipelines (science-ready mosaics, object masks, 2D image decompositions, and stellar mass maps) can be publicly accessed at IRSA (http://irsa.ipac.caltech.edu/data/SPITZER/S4G/).

The Spitzer Survey of Stellar Structure in Galaxies (S^4G) is a deep 3.6 and 4.5 μm imaging survey of 2352 nearby (

We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Ha Fabry Perot (FP) data obtained with the Galaxy Ha Fabry Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Ha. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in Errs format through the NASA/IPAC Extragalactic Database and the Centre de Donnees Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

Background: Deficits in mindfulness-related capacities have been described in borderline personality disorder (BPD). However, little research has been conducted to explore which factors could explain these deficits. This study assesses the relationship between temperamental traits and childhood maltreatment with mindfulness in BPD. Methods: A total of 100 individuals diagnosed with BPD participated in the study. Childhood maltreatment was assessed using the Childhood Trauma Questionnaire (CTQ-SF), temperamental traits were assessed using the Zuckerman-Khulman Personality Questionnaire (ZKPQ), and mindfulness capabilities were evaluated with the Five Facet Mindfulness Questionnaire (FFMQ). Results: Hierarchical regression analyses were performed including only those CTQ-SF and ZKPQ subscales that showed simultaneous significant correlations with mindfulness facets. Results: indicated that neuroticism and sexual abuse were predictors of acting with awareness; and neuroticism, impulsiveness and sexual abuse were significant predictors of non-judging. Temperamental traits did not have a moderator effect on the relationship between childhood sexual abuse and mindfulness facets. Conclusions: These results provide preliminary evidence for the effects of temperamental traits and childhood trauma on mindfulness capabilities in BPD individuals. Further studies are needed to better clarify the impact of childhood traumatic experiences on mindfulness capabilities and to determine the causal relations between these variables.

The Spitzer Survey of Stellar Structure in Galaxies (S(4)G) is a deep 3.6 and 4.5 mu m imaging survey of 2352 nearby (

We present a catalogue and images of visually detected features, such as asymmetries, extensions, warps, shells, tidal tails, polar rings, and obvious signs of mergers or interactions, in the faint outer regions (at and outside of R_25) of nearby galaxies. This catalogue can be used in future quantitative studies that examine galaxy evolution due to internal and external factors. We are able to reliably detect outer region features down to a brightness level of 0.03 MJy/sr per pixel at 3.6 microns in the Spitzer Survey of Stellar Structure in Galaxies (S4G). We also tabulate companion galaxies. We find asymmetries in the outer isophotes in 22+/-1 per cent of the sample. The asymmetry fraction does not correlate with galaxy classification as an interacting galaxy or merger remnant, or with the presence of companions. We also compare the detected features to similar features in galaxies taken from cosmological zoom re-simulations. The simulated images have a higher fraction (33 per cent) of outer disc asymmetries, which may be due to selection effects and an uncertain star formation threshold in the models. The asymmetries may have either an internal (e.g., lopsidedness due to dark halo asymmetry) or external origin., 26 pages, 16 embedded + 100 online-only figures, accepted for publication in MNRAS

Mindfulness has been described as an inherent human capability that can be learned and trained, and its improvement has been associated with better health outcomes in both medicine and psychology. Although the role of practice is central to most mindfulness programs, practice-related improvements in mindfulness skills is not consistently reported and little is known about how the characteristics of meditative practice affect different components of mindfulness. the present study explores the role of practice parameters on self-reported mindfulness skills. A total of 670 voluntary participants with and without previous meditation experience (n = 384 and n = 286, respectively) responded to an internet-based survey on various aspects of their meditative practice (type of meditation, length of session, frequency, and lifetime practice). Participants also completed the Five Facets Mindfulness Questionnaire (FFMQ), and the Experiences Questionnaire (EQ). the group with meditation experience obtained significantly higher scores on all facets of FFMQ and EQ questionnaires compared to the group without experience. However different effect sizes were observed, with stronger effects for the Observing and Non-Reactivity facets of the FFMQ, moderate effects for Decentering in EQ, and a weak effect for Non-judging, Describing, and Acting with awareness on the FFMQ. Our results indicate that not all practice variables are equally relevant in terms of developing mindfulness skills. Frequency and lifetime practice - but not session length or meditation type - were associated with higher mindfulness skills. Given that these 6 mindfulness aspects show variable sensitivity to practice, we created a composite index (MINDSENS) consisting of those items from FFMQ and EQ that showed the strongest response to practice. the MINDSENS index was able to correctly discriminate daily meditators from non-meditators in 82.3% of cases. These findings may contribute to the understanding of the development of mindfulness skills and support trainers and researchers in improving mindfulness-oriented practices and programs. Hosp Santa Creu St Pau, Dept Psychiat, Barcelona, Spain Univ Autonoma Barcelona, CIBERSAM, IIB ST PAU, E-08193 Barcelona, Spain Ciber Fisiopatol Obesidad Nutr CIBERO, Santiago de Compostela, Spain Univ Jaume 1, Dept Psicol Basica Clin Psicobiol, Castellon de La Plana, Spain Universidade Federal de São Paulo, Dept Prevent Med, Mente Aberta Brazilian Ctr Mindfulness & Hlth Pro, São Paulo, Brazil Univ Valencia, Dept Personalitat Avaluacio Tractaments Psicol, Valencia, Spain Miguel Servet Hosp, Dept Psychiat, Zaragoza, Spain Univ Zaragoza, Inst Aragones Ciencias Salud, REDIAPP, Zaragoza, Spain Universidade Federal de São Paulo, Dept Prevent Med, Mente Aberta Brazilian Ctr Mindfulness & Hlth Pro, São Paulo, Brazil Web of Science

We present a new approach for estimating the 3.6 mu m stellar mass-to-light (M/L) ratio Rho 3.6 in terms of the [3.6]-[4.5] colors of old stellar populations. Our approach avoids several of the largest sources of uncertainty in existing techniques using population synthesis models. By focusing on mid-IR wavelengths, we gain a virtually dust extinction-free tracer of the old stars, avoiding the need to adopt a dust model to correctly interpret optical or optical/near-IR colors normally leveraged to assign the mass-to-light ratio.. By calibrating a new relation between near-IR and mid-IR colors of giant stars observed in GLIMPSE we also avoid the discrepancies in model predictions for the [3.6]-[4.5] colors of old stellar populations due to uncertainties in the molecular line opacities assumed in template spectra. We find that the [3.6]-[4.5] color, which is driven primarily by metallicity, provides a tight constraint on.3.6, which varies intrinsically less than at optical wavelengths. The uncertainty on.3.6 of similar to 0.07 dex due to unconstrained age variations marks a significant improvement on existing techniques for estimating the stellar M/L with shorter wavelength data. A single.3.6 = 0.6 (assuming a Chabrier initial mass function (IMF)), independent of [3.6]-[4.5] color, is also feasible because it can be applied simultaneously to old, metal-rich and young, metal-poor populations, and still with comparable (or better) accuracy (similar to 0.1 dex) than alternatives. We expect our.3.6 to be optimal formapping the stellarmass distributions in S(4)G galaxies, for which we have developed an independent component analysis technique to first isolate the old stellar light at 3.6 mu m from nonstellar emission (e. g., hot dust and the 3.3 polycyclic aromatic hydrocarbon feature). Our estimate can also be used to determine the fractional contribution of nonstellar emission to global (rest-frame) 3.6 mu m fluxes, e.g., in WISE imaging, and establishes a reliable basis for exploring variations in the stellar IMF.

Documento de registro personal de prácticas clínicas para los estudiantes de Grado en Enfermería de la Universidad de Cádiz., Documento de registro de prácticas clínicas para los estudiantes de Grado en Enfermería. Basado en el aprendizaje reflexivo. El documento es único para todo el practicum, de manera que el estudiante va cumplimentándolo y realizando las actividades solicitadas en cada curso. Incluye un apartado de requisitos, recomendaciones y normas y el listado de actividades y tareas a realizar por cada curso académico. Además introduce en cada bloque de actividades, un apartado para la reflexión personal del estudiante., Documento de 36 páginas, en formato word.

We study the m = 1 distortions (lopsidedness) in the stellar components of 167 nearby galaxies that span a wide range of morphologies and luminosities. We confirm the previous findings of (1) a high incidence of lopsidedness in the stellar distributions, (2) increasing lopsidedness as a function of radius out to at least 3.5 exponential scale lengths, and (3) greater lopsidedness, over these radii, for galaxies of later type and lower surface brightness. Additionally, the magnitude of the lopsidedness (1) correlates with the character of the spiral arms (stronger arm patterns occur in galaxies with less lopsidedness), (2) is not correlated with the presence or absence of a bar, or the strength of the bar when one is present, (3) is inversely correlated to the stellar mass fraction, f(*), within one radial scale length, and (4) correlates directly with f(*) measured within the radial range over which we measure lopsidedness. We interpret these findings to mean that lopsidedness is a generic feature of galaxies and does not, generally, depend on a rare event, such as a direct accretion of a satellite galaxy onto the disk of the parent galaxy. While lopsidedness may be caused by several phenomena, moderate lopsidedness (< A1 >(i) + < A(1)>(o))/2 < 0.3) is likely to reflect halo asymmetries to which the disk responds or a gravitationally self-generated mode. We hypothesize that the magnitude of the stellar response depends both on how centrally concentrated the stars are with respect to the dark matter and whether there are enough stars in the region of the lopsidedness that self-gravity is dynamically important.

Stellar bars can lead to gas inflow toward the center of a galaxy and stimulate nuclear star formation. However, there is no compelling evidence on whether they also feed a central supermassive black hole: by measuring the fractions of barred active and inactive galaxies, previous studies have yielded conflicting results. In this paper, we aim to understand the lack of observational evidence for bar-driven active galactic nucleus (AGN) activity by studying a sample of 41 nearby (d < 35 Mpc) barred galaxies from the Spitzer Survey for Stellar Structure in Galaxies. We use Chandra observations to measure nuclear 2-10 keV X-ray luminosities and estimate Eddington ratios, together with Spitzer 3.6 mu m imaging to quantify the strength of the stellar bar in two independent ways: (1) from its structure, as traced by its ellipticity and boxiness, and (2) from its gravitational torque Q(b), taken as the maximum ratio of the tangential force to the mean background radial force. In this way, rather than discretizing the presence of both stellar bars and nuclear activity, we are able to account for the continuum of bar strengths and degrees of AGN activity. We find nuclear X-ray sources in 31 out of 41 galaxies with median X-ray luminosity and Eddington ratio of L-X = 4.3 x 10(38) erg s(-1) and L-bol/L-Edd = 6.9 x 10(-6), respectively, consistent with low-luminosity AGN activity. Including upper limits for those galaxies without nuclear detections, we find no significant correlation between any of the bar strength indicators and the degree of nuclear activity, irrespective of galaxy luminosity, stellar mass, Hubble type, or bulge size. Strong bars do not favor brighter or more efficient nuclear activity, implying that at least for the low-luminosity regime, supermassive black hole fueling is not closely connected to large-scale features.

We have analyzed the radial distribution of old stars in a sample of 218 nearby face-on disks, using deep 3.6 mu m images from the Spitzer Survey of Stellar Structure in Galaxies. In particular, we have studied the structural properties of those disks with a broken or down-bending profile. We find that, on average, disks with a genuine single-exponential profile have a scale length and a central surface brightness which are intermediate to those of the inner and outer components of a down-bending disk with the same total stellar mass. In the particular case of barred galaxies, the ratio between the break and the bar radii (R-br/R-bar) depends strongly on the total stellar mass of the galaxy. For galaxies more massive than 10(10) M-circle dot, the distribution is bimodal, peaking at R-br/R-bar similar to 2 and similar to 3.5. The first peak, which is the most populated one, is linked to the outer Lindblad resonance of the bar, whereas the second one is consistent with a dynamical coupling between the bar and the spiral pattern. For galaxies below 10(10) M-circle dot, breaks are found up to similar to 10 R-bar, but we show that they could still be caused by resonances given the rising nature of rotation curves in these low-mass disks. While not ruling out star formation thresholds, our results imply that radial stellar migration induced by non-axisymmetric features can be responsible not only for those breaks at similar to 2 R-bar, but also for many of those found at larger radii.

Background: The Borderline Symptom List-23 (BSL-23) is a reliable and valid self-report instrument for assessing Borderline Personality Disorder (BPD) severity. The psychometric properties of the original version have proven to be adequate. The aim of the present study was to validate the Spanish language version of the BSL-23. Methods: The BSL-23 was administered to 240 subjects with BPD diagnosis. Factor structure, reliability, test-retest stability, convergent validity, and sensitivity to change were analyzed. Results: The Spanish version of the BSL-23 replicates the one-factor structure of the original version. The scale has high reliability (Cronbach's alpha=.949), as well as good test-retest stability, which was checked in a subsample (n=74; r=.734; p

We have performed two-dimensional multicomponent decomposition of 144 local barred spiral galaxies using 3.6 $��{\rm m}$ images from the Spitzer Survey of Stellar Structure in Galaxies. Our model fit includes up to four components (bulge, disk, bar, and a point source) and, most importantly, takes into account disk breaks. We find that ignoring the disk break and using a single disk scale length in the model fit for Type II (down-bending) disk galaxies can lead to differences of 40% in the disk scale length, 10% in bulge-to-total luminosity ratio (B/T), and 25% in bar-to-total luminosity ratios. We find that for galaxies with B/T $\geq$ 0.1, the break radius to bar radius, $r_{\rm br}/R_{\rm bar}$, varies between 1 and 3, but as a function of B/T the ratio remains roughly constant. This suggests that in bulge-dominated galaxies the disk break is likely related to the outer Lindblad Resonance (OLR) of the bar, and thus moves outwards as the bar grows. For galaxies with small bulges, B/T $, Accepted for publication in ApJ, 21 pages, 13 figures, 2 tables

The mechanism causing breaks in the radial surface brightness distribution of spiral galaxies is not yet well known. Despite theoretical efforts, there is not a unique explanation for these features and the observational results are not conclusive. In an attempt to address this problem, we have selected a sample of 34 highly inclined spiral galaxies present both in the Sloan Digital Sky Survey and in the Spitzer Survey of Stellar Structure in Galaxies. We have measured the surface brightness profiles in the five Sloan optical bands and in the 3.6$\mu m$ Spitzer band. We have also calculated the color and stellar surface mass density profiles using the available photometric information, finding two differentiated features: an innermost break radius at distances of $\sim 8 \pm 1$ kpc [$0.77 \pm 0.06$ $R_{25}$] and a second characteristic radius, or truncation radius, close to the outermost optical extent ($\sim 14 \pm 2$ kpc [$1.09 \pm 0.05$ $R_{25}$]) of the galaxy. We propose in this work that the breaks might be a phenomena related to a threshold in the star formation, while truncations are more likely a real drop in the stellar mass density of the disk associated with the maximum angular momentum of the stars., Comment: 15 pages, 13 figures and 5 tables (+ appendix). Accepted for publication in MNRAS

We present a study of the kinematics of the isolated spiral galaxy NGC 864, using H{\alpha} Fabry-Perot data obtained with the GH{\alpha}FaS instrument at the William Herschel Telescope in La Palma, complemented with images at 3.6 {\mu}m, in the R band and in H{\alpha} filter, and integral field spectroscopic data. The resulting data cubes and velocity maps allow the study of the kinematics of the galaxy, including in-depth investigations of the rotation curve, velocity moment maps, velocity residual maps, gradient maps and position-velocity diagrams. We find asymmetries in the velocity field in the bar zone, caused by non-circular motions, probably in response to the potential of the bar. We also find a flat-profile bar, in agreement with the strong bar, with the grand design spiral pattern, and with the gap between the ends of the bar and the start of the spiral arms. We quantify the rate of massive star formation, which is concentrated in the two spiral arms., Comment: 14 pages, 11 figures, 2 tables

Tidal debris around galaxies can yield important clues on their evolution. We have identified tidal debris in 11 early-type galaxies (T ≤ 0) from a sample of 65 early types drawn from the Spitzer Survey of Stellar Structure in Galaxies (S4G). The tidal debris includes features such as shells, ripples, and tidal tails. A variety of techniques, including two-dimensional decomposition of galactic structures, were used to quantify the residual tidal features. The tidal debris contributes ~3%-10% to the total 3.6 μm luminosity of the host galaxy. Structural parameters of the galaxies were estimated using two-dimensional profile fitting. We investigate the locations of galaxies with tidal debris in the fundamental plane and Kormendy relation. We find that galaxies with tidal debris lie within the scatter of early-type galaxies without tidal features. Assuming that the tidal debris is indicative of recent gravitational interaction or merger, this suggests that these galaxies have either undergone minor merging events so that the overall structural properties of the galaxies are not significantly altered, or they have undergone a major merging events but already have experienced sufficient relaxation and phase mixing so that their structural properties become similar to those of the non-interacting early-type galaxies.

FUNDAMENTO: A estimulação endocárdica convencional do ventrículo direito (VD) ocasiona alargamento do QRS e dessincronização do miocárdio, comprometendo a função ventricular. Com a necessidade de estimulação menos deletéria, a estimulação septal do VD tem sido mais utilizada. Eventualmente têm sido relatados limiares mais altos e ondas R menores na estimulação septal. OBJETIVO: Comparar os parâmetros das estimulações apical e septal, intrapaciente, para verificar se existem diferenças que possam interferir na escolha do ponto de estimulação. MÉTODOS: Estudo prospectivo controlado. Foram incluídos 25 pacientes, com 67,2 ± 9 anos, 10 (40%) mulheres, com indicações de marca-passo por bradiarritmias. Etiologias foram degenerativa em nove (36%), coronariopatia em oito (32%), doença de Chagas em sete (28%), e valvopatia em um (4%) pacientes. Foram utilizados eletrodos de fixação ativa e avaliados os limiares de comando, impedância e onda R uni e bipolares no implante e após seis meses. RESULTADOS: A média aguda dos limiares de comando, ondas R e impedâncias unipolares/bipolares septais x apicais foram, respectivamente, 0,73x0,74V e 0,73x0,78V; 10x9,9 mV e 12,3x12,4 mV; 579x621 Ω e 611x629 Ω. Comparações entre parâmetros septais e apicais com teste t-pareado bicaudal demonstraram um P > 0,1. Após seis meses, a média dos limiares de comando, ondas R e Impedâncias unipolares/ bipolares septais x apicais foram, respectivamente, 0,5 x 0,72 V e 0,71 x 0,87 V; 11,4x9,5 mV e 12x11,2 mV; 423x426Ω e 578x550Ω, com P > 0,05, exceto comparando-se limiar de estimulação unipolar septal com apical unipolar p de 0,02. CONCLUSÃO: Utilizando comparações intrapaciente, não existem diferenças expressivas entre parâmetros eletrofisiológicos de estimulação septal e apical sendo que não há restrições para a escolha da estimulação septal em ventrículo direito.

We examine the effect of circumstellar dust extinction on the near-IR contribution of asymptotic giant branch (AGB) stars in intermediate-age clusters throughout the disk of M100. For our sample of 17 AGB-dominated clusters we extract optical-to-mid-IR SEDs and find that NIR brightness is coupled to the mid-IR dust emission in such a way that a significant reduction of AGB light, of up to 1 mag in K-band, follows from extinction by the dust shell formed during this stage. Since the dust optical depth varies with AGB chemistry (C-rich or O-rich), our results suggest that the contribution of AGB stars to the flux from their host clusters will be closely linked to the metallicity and the progenitor mass of the AGB star, to which dust chemistry and mass-loss rate are sensitive. Our sample of clusters--each the analogue of a ~1 Gyr old post-starburst galaxy--has implications within the context of mass and age estimation via SED modelling at high z: we find that the average ~0.5 mag extinction estimated here may be sufficient to reduce the AGB contribution in (rest-frame) K-band from ~70%, as predicted in the latest generation of synthesis models, to ~35%. Our technique for selecting AGB-dominated clusters in nearby galaxies promises to be effective for discriminating the uncertainties associated with AGB stars in intermediate-age populations that plague age and mass estimation in high-z galaxies., 6 pages, 4 figures, 1 table, accepted for publication in ApJL

We examine the effect of circumstellar dust extinction on the near-IR (NIR) contribution of asymptotic giant branch (AGB) stars in intermediate-age clusters throughout the disk of M100. For our sample of 17AGB-dominated clusters we extract optical-to-mid-IR spectral energy distributions (SEDs) and find that NIR brightness is coupled to the mid-IR dust emission in such a way that a significant reduction of AGB light, of up to 1 mag in the K band, follows from extinction by the dust shell formed during this stage. Since the dust optical depth varies with AGB chemistry (C-rich or O-rich), our results suggest that the contribution of AGB stars to the flux from their host clusters will be closely linked to the metallicity and the progenitor mass of the AGB star, to which dust chemistry and mass-loss rate are sensitive. Our sample of clusters-each the analogue of a similar to 1 Gyr old post-starburst galaxy-has implications within the context of mass and age estimation via SED modeling at high-z: we find that the average similar to 0.5 mag extinction estimated here may be sufficient to reduce the AGB contribution in the (rest-frame) K band from similar to 70%, as predicted in the latest generation of synthesis models, to similar to 35%. Our technique for selecting AGB-dominated clusters in nearby galaxies promises to be effective for discriminating the uncertainties associated with AGB stars in intermediate-age populations that plague age and mass estimation in high-z galaxies.

With the aim of constructing accurate two-dimensional maps of the stellar mass distribution in nearby galaxies from Spitzer Survey of Stellar Structure in Galaxies 3.6 and 4.5 mu m images, we report on the separation of the light from old stars from the emission contributed by contaminants. Results for a small sample of six disk galaxies (NGC 1566, NGC 2976, NGC 3031, NGC 3184, NGC 4321, and NGC 5194) with a range of morphological properties, dust content, and star formation histories are presented to demonstrate our approach. To isolate the old stellar light from contaminant emission (e.g., hot dust and the 3.3 mu m polycyclic aromatic hydrocarbon (PAH) feature) in the IRAC 3.6 and 4.5 mu m bands we use an independent component analysis (ICA) technique designed to separate statistically independent source distributions, maximizing the distinction in the [3.6]-[4.5] colors of the sources. The technique also removes emission from evolved red objects with a low mass-to-light ratio, such as asymptotic giant branch (AGB) and red supergiant (RSG) stars, revealing maps of the underlying old distribution of light with [3.6]-[4.5] colors consistent with the colors of K and M giants. The contaminants are studied by comparison with the non-stellar emission imaged at 8 mu m, which is dominated by the broad PAH feature. Using the measured 3.6 mu m/8 mu m ratio to select individual contaminants, we find that hot dust and PAHs together contribute between similar to 5% and 15% to the integrated light at 3.6 mu m, while light from regions dominated by intermediate-age (AGB and RSG) stars accounts for only 1%-5%. Locally, however, the contribution from either contaminant can reach much higher levels; dust contributes on average 22% to the emission in star-forming regions throughout the sample, while intermediate-age stars contribute upward of 50% in localized knots. The removal of these contaminants with ICA leaves maps of the old stellar disk that retain a high degree of structural information and are ideally suited for tracing stellar mass, as will be the focus in a companion paper.

With the aim of constructing accurate 2D maps of the stellar mass distribution in nearby galaxies from S4G 3.6 and 4.5 micron images, we report on the separation of the light from old stars from the emission contributed by contaminants (e.g. hot dust and the 3.3 micron PAH feature). Results for a small sample of six disk galaxies (NGC 1566, NGC 2976, NGC 3031, NGC 3184, NGC 4321, and NGC 5194) with a range of morphological properties, dust contents and star formation histories are presented to demonstrate our approach. We use an Independent Component Analysis (ICA) technique designed to separate statistically independent source distributions, maximizing the distinction in the [3.6]-[4.5] colors of the sources. The technique also removes emission from intermediate-age evolved red objects with a low mass-to-light ratio, such as asymptotic giant branch (AGB) and red supergiant (RSG) stars, revealing maps of the underlying old distribution of light with [3.6]-[4.5] colors consistent with the colors of K and M giants. Contaminants are identified via comparison to the non-stellar emission imaged at 8 microns, which is dominated by the broad PAH feature. Using the measured 3.6/8 micron ratio to select the individual contaminants, we find that hot dust and PAH together contribute between ~5-15% to the integrated light at 3.6 microns, while light from regions dominated by intermediate-age stars accounts for only 1-5%. Locally, however, the contribution from either contaminant can reach much higher levels; dust contributes on average 22% to the emission in star-forming regions throughout the sample, while intermediate age-stars contribute upwards of 50% in localized knots. The removal of these contaminants with ICA leaves maps of the old stellar disk that retain a high degree of structural information and are ideally suited for tracing the stellar mass, as will be the focus in a companion paper., 19 pages, 5 figures, accepted for publication in ApJ

Junta de Andalucía PO7-SEJ-2564 Ministerio de Educación y Ciencia SEJ2007-66487/GEOG

Spiral arm properties of 46 galaxies in the Spitzer Survey of Stellar Structure in Galaxies (S(4)G) were measured at 3.6 mu m, where extinction is small and the old stars dominate. The sample includes flocculent, multiple arm, and grand design types with a wide range of Hubble and bar types. We find that most optically flocculent galaxies are also flocculent in the mid-IR because of star formation uncorrelated with stellar density waves, whereas multiple arm and grand design galaxies have underlying stellar waves. Arm-interarm contrasts increase from flocculent to multiple arm to grand design galaxies and with later Hubble types. Structure can be traced further out in the disk than in previous surveys. Some spirals peak at mid-radius while others continuously rise or fall, depending on Hubble and bar type. We find evidence for regular and symmetric modulations of the arm strength in NGC 4321. Bars tend to be long, high amplitude, and flat-profiled in early-type spirals, with arm contrasts that decrease with radius beyond the end of the bar, and they tend to be short, low amplitude, and exponential-profiled in late Hubble types, with arm contrasts that are constant or increase with radius. Longer bars tend to have larger amplitudes and stronger arms.

Most, if not all, disk galaxies have a thin (classical) disk and a thick disk. In most models thick disks are thought to be a necessary consequence of the disk formation and/or evolution of the galaxy. We present the results of a study of the thick disk properties in a sample of carefully selected edge-on galaxies with types ranging from T = 3 to T = 8. We fitted one-dimensional luminosity profiles with physically motivated functions-the solutions of two stellar and one gaseous isothermal coupled disks in equilibrium-which are likely to yield more accurate results than other functions used in previous studies. The images used for the fits come from the Spitzer Survey of Stellar Structure in Galaxies (S(4)G). We found that thick disks are on average more massive than previously reported, mostly due to the selected fitting function. Typically, the thin and thick disks have similar masses. We also found that thick disks do not flare significantly within the observed range in galactocentric radii and that the ratio of thick-to-thin disk scale heights is higher for galaxies of earlier types. Our results tend to favor an in situ origin for most of the stars in the thick disk. In addition, the thick disk may contain a significant amount of stars coming from satellites accreted after the initial buildup of the galaxy and an extra fraction of stars coming from the secular heating of the thin disk by its own overdensities. Assigning thick disk light to the thin disk component may lead to an underestimate of the overall stellar mass in galaxies because of different mass-to-light ratios in the two disk components. On the basis of our new results, we estimate that disk stellar masses are between 10% and 50% higher than previously thought and we suggest that thick disks are a reservoir of “local missing baryons.”

Resumen tomado de la publicación Una de las principales dificultades en la investigación de las emociones es la inducción de una respuesta emocional real mediante técnicas artificiales. El objetivo del presente estudio es validar al español una batería de películas con capacidad para inducir emociones (PIE) bajo condiciones experimentales y analizar su capacidad para provocar emociones básicas diferenciadas. Una muestra de 127 sujetos participaron en el estudio, se utilizaron 57 escenas de películas dobladas al español con capacidad en estudios previos para inducir 7 emociones: ira, miedo, tristeza, asco, diversión, ternura y neutra. La respuesta emocional subjetiva se midió utilizando la Self Assessment Manikins y el Discrete Emotions Questionnaire. Las películas mostraron una buena capacidad para inducir afectos positivos y negativos, niveles elevados de activación emocional y variaciones en la percepción de control de la emoción. Permitían la inducción de las emociones básicas de diversión y miedo diferenciadas, sin embargo, las de tristeza y asco no se diferenciaban significativamente de las de ira, y las de ira y ternura de las de tristeza. La PIE puede ser una herramienta útil para la investigación experimental de las emociones en población española. Asturias Colegio Oficial de Psicólogos de Asturias; Calle Ildefonso Sánchez del Río, 4-1 B; 33001 Oviedo; Tel. +34985285778; Fax +34985281374; Universidad de Oviedo. Facultad de Psicología; Plaza Feijoo, s. n.; 33003 Oviedo; Tel. +34985104146; Fax +34985104126; ESP

The Spitzer Survey of Stellar Structure in Galaxies S^4G is an Exploration Science Legacy Program approved for the Spitzer post-cryogenic mission. It is a volume-, magnitude-, and size-limited (d < 40 Mpc, |b| > 30 degrees, m_(Bcorr) < 15.5, D25>1') survey of 2,331 galaxies using IRAC at 3.6 and 4.5 microns. Each galaxy is observed for 240 s and mapped to > 1.5 x D25. The final mosaicked images have a typical 1 sigma rms noise level of 0.0072 and 0.0093 MJy / sr at 3.6 and 4.5 microns, respectively. Our azimuthally-averaged surface brightness profile typically traces isophotes at mu_3.6 (AB) (1 sigma) ~ 27 mag arcsec^-2, equivalent to a stellar mass surface density of ~ 1 Msun pc^-2. S^4G thus provides an unprecedented data set for the study of the distribution of mass and stellar structures in the local Universe. This paper introduces the survey, the data analysis pipeline and measurements for a first set of galaxies, observed in both the cryogenic and warm mission phase of Spitzer. For every galaxy we tabulate the galaxy diameter, position angle, axial ratio, inclination at mu_3.6 (AB) = 25.5 and 26.5 mag arcsec^-2 (equivalent to ~ mu_B (AB) =27.2 and 28.2 mag arcsec^-2, respectively). These measurements will form the initial S^4G catalog of galaxy properties. We also measure the total magnitude and the azimuthally-averaged radial profiles of ellipticity, position angle, surface brightness and color. Finally, we deconstruct each galaxy using GALFIT into its main constituent stellar components: the bulge/spheroid, disk, bar, and nuclear point source, where necessary. Together these data products will provide a comprehensive and definitive catalog of stellar structures, mass and properties of galaxies in the nearby Universe., Accepted for Publication in PASP, 14 pages, 13 figures

Spitzer Space Telescope Infrared Array Camera imaging provides an opportunity to study all known morphological types of galaxies in the mid-IR at a depth significantly better than ground-based near-infrared and optical images. The goal of this study is to examine the imprint of the de Vaucouleurs classification volume in the 3.6 μm band, which is the best Spitzer waveband for galactic stellar mass morphology owing to its depth and its reddening-free sensitivity mainly to older stars. For this purpose, we have prepared classification images for 207 galaxies from the Spitzer archive, most of which are formally part of the Spitzer Survey of Stellar Structure in Galaxies (S^4G), a Spitzer post-cryogenic ("warm") mission Exploration Science Legacy Program survey of 2331 galaxies closer than 40 Mpc. For the purposes of morphology, the galaxies are interpreted as if the images are blue light, the historical waveband for classical galaxy classification studies. We find that 3.6 μm classifications are well correlated with blue-light classifications, to the point where the essential features of many galaxies look very similar in the two very different wavelength regimes. Drastic differences are found only for the most dusty galaxies. Consistent with a previous study by Eskridge et al., the main difference between blue-light and mid-IR types is an ≈1 stage interval difference for S0/a to Sbc or Sc galaxies, which tend to appear "earlier" in type at 3.6 μm due to the slightly increased prominence of the bulge, the reduced effects of extinction, and the reduced (but not completely eliminated) effect of the extreme population I stellar component. We present an atlas of all of the 207 galaxies analyzed here and bring attention to special features or galaxy types, such as nuclear rings, pseudobulges, flocculent spiral galaxies, I0 galaxies, double-stage and double-variety galaxies, and outer rings, that are particularly distinctive in the mid-IR.

El objetivo principal de esta tesis consiste en cuantificar la distribución espacial de las propiedades físicas de las estrellas, el gas y el polvo en galaxias cercanas, dado que son el registro fósil de su evolución pasada. En particular, nos centraremos sobre todo en las variaciones de estas propiedades con la distancia al centro de las galaxias espirales.[ABSTRACT]The main goal of this thesis is to quantify the spatial distribution of the physical properties of stars, gas and dust in nearby galaxies, since they are the fossil record of their past evolution. In particular, we will mostly focus on the variations of these properties with the galactocentric distance in spiral galaxies.

The lntegrated Maritime Policy (IMP) of the EU is included within the new maritime policy initiatives arisen in the last years both in developed and developing countries. This article claims that these initiatives are the response to the new challenges in the oceanic domain. The lMP is the European answer to the new oceanic order. In the global context, the lMP competes with other emerging countries with dynamic economies, whose competitiveness rests on not so rigorous social and environmental standards. On the other hand, this article underlines the importance of maritime policies for security, as they contribute to a better governance of the oceanic domain which, to a great extent, Jalls outside the jurisdiction of the States.

Spitzer Space Telescope Infrared Array Camera (IRAC) imaging provides an opportunity to study all known morphological types of galaxies in the mid-IR at a depth significantly better than ground-based near-infrared and optical images. The goal of this study is to examine the imprint of the de Vaucouleurs classification volume in the 3.6 micron band, which is the best Spitzer waveband for galactic stellar mass morphology owing to its depth and its reddening-free sensitivity mainly to older stars. For this purpose, we have prepared classification images for 207 galaxies from the Spitzer archive, most of which are formally part of the Spitzer Survey of Stellar Structure in Galaxies (S^4G), a Spitzer post-cryogenic ("warm") mission Exploration Science Legacy Program survey of 2,331 galaxies closer than 40 Mpc. For the purposes of morphology, the galaxies are interpreted as if the images are {\it blue light}, the historical waveband for classical galaxy classification studies. We find that 3.6 micron classifications are well-correlated with blue-light classifications, to the point where the essential features of many galaxies look very similar in the two very different wavelength regimes. Drastic differences are found only for the most dusty galaxies. Consistent with a previous study by Eskridge et al. (2002), the main difference between blue light and mid-IR types is an approximately 1 stage interval difference for S0/a to Sbc or Sc galaxies, which tend to appear "earlier" in type at 3.6 microns due to the slightly increased prominence of the bulge, the reduced effects of extinction, and the reduced (but not completely eliminated) effect of the extreme population I stellar component. We present an atlas of all of the 207 galaxies analyzed here, and bring attention to special features or galaxy types that are particularly distinctive in the mid-IR., Comment: Accepted for publication in the Astrophysical Journal Supplement Series (LaTex, 269 pages + 211 figures, uses aastex.cls); for a higher resolution pdf, see http://bama.ua.edu/~rbuta/s4g/. For the atlas of images and notes only, see http://bama.ua.edu/~rbuta/s4gatlas/

Desde la aprobación de la Ley de los Océanos (1996), Canadá ha sido considerado una referencia internacional en el proceso de construcción de un nuevo paradigma oceánico basado en una visión integrada y omnicompresiva del mar. Su estudio permite contrastar en que medida la descentralización político-territorial se extiende al gobierno de lo marítimo. La aproximación a las problemáticas vinculadas a la gestión federal y provincial de las áreas marinas y a las modalidades con que se están elaborando modelos viables de planificación, puede constituir un aporte valioso para otras iniciativas nacionales. Se sostiene la hipótesis que en un Estado descentralizado, en el cual cabría esperar que la descentralización se extendiese a las cuestiones marinas, se constata cierta reticencia a devolver a las varias unidades político-territoriales los poderes de administración del área oceánica. Esta se constituiría así en el último baluarte de la fortaleza soberana de la autoridad nacional., Since the adoption of its Oceans Act (1996), Canada has been regarded as an international point of reference and the model to adhere to in the new ocean paradigm construction process based on the creation of an integrated and all-embracing vision of the marine environment. Its study Act allows the degree to which political and territorial decentralisation extends to the governance of maritime affairs to be contrasted. Its approach to all the problems surrounding federal and provincial governance of marine areas and the methods being used to devise viable planning models might constitute a valuable contribution for initiatives in other nations. The hypothesis put forward here is that in a decentralised State, where it might be supposed that decentralisation would extend to marine affairs, a certain reticence towards devolving the powers to manage the area of the ocean to the different political and territorial units can be seen to exist. This would therefore be the last bastion of the sovereign fortress of national authority.

Desde la aprobación de la Ley de los Océanos (1996), Canadá ha sido considerado una referencia internacional en el proceso de construcción de un nuevo paradigma oceánico basado en una visión integrada y omnicompresiva del mar. Su estudio permite contrastar en que medida la descentralización político-territorial se extiende al gobierno de lo marítimo. La aproximación a las problemáticas vinculadas a la gestión federal y provincial de las áreas marinas y a las modalidades con que se están elaborando modelos viables de planificación, puede constituir un aporte valioso para otras iniciativas nacionales. Se sostiene la hipótesis que en un Estado descentralizado, en el cual cabría esperar que la descentralización se extendiese a las cuestiones marinas, se constata cierta reticencia a devolver a las varias unidades político-territoriales los poderes de administración del área oceánica. Esta se constituiría así en el último baluarte de la fortaleza soberana de la autoridad nacional. Since the adoption of its Oceans Act (1996), Canada has been regarded as an international point of reference and the model to adhere to in the new ocean paradigm construction process based on the creation of an integrated and all-embracing vision of the marine environment. Its study Act allows the degree to which political and territorial decentralisation extends to the governance of maritime affairs to be contrasted. Its approach to all the problems surrounding 2 federal and provincial governance of marine areas and the methods being used to devise viable planning models might constitute a valuable contribution for initiatives in other nations. The hypothesis put forward here is that in a decentralised State, where it might be supposed that decentralisation would extend to marine affairs, a certain reticence towards devolving the powers to manage the area of the ocean to the different political and territorial units can be seen to exist. This would therefore be the last bastion of the sovereign fortress of national authority.

La Política Marítma Integrada (PMI) de la UE se inserta en la corriente de iniciativas de nuevas políticas marítimas surgidas en los úlitmos años tanto en países desarrollados como en desarrollo. En este artículo se mantiene que estas iniciativas constituyen la respuesta a nuevos desafíos en el ámbito oceánico. La PMI se puede interpretar como la respuesta de la UE a este nuevo orden oceánico. En el contexto global, la PMI se ve impelida a competir con los países que protagonizan el mayor dinamismo económico y que basan su competitividad en estándares sociales y medioambientales de menor exigencia. Por otra parte, el artículo pone de manifiesto cómo las políticas marítimas son fundamentales para la seguridad , en la medida en que coadyuvan a una mejor gobernanza de un ámbito como el oceánico, que en una alta proporción se sitúa fuera de la jurisdicción de los Estados.