The age and abundance structure of the stellar populations in the central sub-kpc of the Milky Way

The four main findings about the age and abundance structure of the Milky Way bulge based on microlensed dwarf and subgiant stars are: (1) a wide metallicity distribution with distinct peaks at [Fe/H]=-1.09, -0.63, -0.20, +0.12, +0.41; (2) a high fraction of intermediate-age to young stars where at [Fe/H]>0 more than 35 % are younger than 8 Gyr, (3) several episodes of significant star formation in the bulge 3, 6, 8, and 11 Gyr ago; (4) the `knee' in the alpha-element abundance trends of the sub-solar metallicity bulge appears to be located at a slightly higher [Fe/H] (about 0.05 to 0.1 dex) than in the local thick disk.Comment: 4 pages, contributed talk at the IAU Symposium 334 "Rediscovering our Galaxy" in Potsdam, July 10-14, 201

Chemical similarities between Galactic bulge and local thick disk red giant stars

The evolution of the Milky Way bulge and its relationship with the other Galactic populations is still poorly understood. The bulge has been suggested to be either a merger-driven classical bulge or the product of a dynamical instability of the inner disk. To probe the star formation history, the initial mass function and stellar nucleosynthesis of the bulge, we performed an elemental abundance analysis of bulge red giant stars. We also completed an identical study of local thin disk, thick disk and halo giants to establish the chemical differences and similarities between the various populations. High-resolution infrared spectra of 19 bulge giants and 49 comparison giants in the solar neighborhood were acquired with Gemini/Phoenix. All stars have similar stellar parameters but cover a broad range in metallicity. A standard 1D local thermodynamic equilibrium analysis yielded the abundances of C, N, O and Fe. A homogeneous and differential analysis of the bulge, halo, thin disk and thick disk stars ensured that systematic errors were minimized. We confirm the well-established differences for [O/Fe] (at a given metallicity) between the local thin and thick disks. For the elements investigated, we find no chemical distinction between the bulge and the local thick disk, which is in contrast to previous studies relying on literature values for disk dwarf stars in the solar neighborhood. Our findings suggest that the bulge and local thick disk experienced similar, but not necessarily shared, chemical evolution histories. We argue that their formation timescales, star formation rates and initial mass functions were similar.Comment: Accepted for publication in A&A, 5 page

Exploring the Dust Content of Galactic Winds with Herschel. I. NGC 4631

We present a detailed analysis of deep far-infrared observations of the nearby edge-on star-forming galaxy NGC 4631 obtained with the Herschel Space Observatory. Our PACS images at 70 and 160 um show a rich complex of filaments and chimney-like features that extends up to a projected distance of 6 kpc above the plane of the galaxy. The PACS features often match extraplanar Halpha, radio-continuum, and soft X-ray features observed in this galaxy, pointing to a tight disk-halo connection regulated by star formation. On the other hand, the morphology of the colder dust component detected on larger scale in the SPIRE 250, 350, and 500 um data matches the extraplanar H~I streams previously reported in NGC 4631 and suggests a tidal origin. The PACS 70/160 ratios are elevated in the central ~3.0 kpc region above the nucleus of this galaxy (the "superbubble"). A pixel-by-pixel analysis shows that dust in this region has a higher temperature and/or an emissivity with a steeper spectral index (beta > 2) than the dust in the disk, possibly the result of the harsher environment in the superbubble. Star formation in the disk seems energetically insufficient to lift the material out of the disk, unless it was more active in the past or the dust-to-gas ratio in the superbubble region is higher than the Galactic value. Some of the dust in the halo may also have been tidally stripped from nearby companions or lifted from the disk by galaxy interactions.Comment: Accepted for publication in The Astrophysical Journa

Searching for the signatures of terrestial planets in solar analogs

We present a fully differential chemical abundance analysis using very high-resolution (R >~ 85,000) and very high signal-to-noise (S/N~800 on average) HARPS and UVES spectra of 7 solar twins and 95 solar analogs, 24 are planet hosts and 71 are stars without detected planets. The whole sample of solar analogs provide very accurate Galactic chemical evolution trends in the metalliciy range -0.3<[Fe/H]<0.5. Solar twins with and without planets show similar mean abundance ratios. We have also analysed a sub-sample of 28 solar analogs, 14 planet hosts and 14 stars without known planets, with spectra at S/N~850 on average, in the metallicity range 0.14<[Fe/H]<0.36 and find the same abundance pattern for both samples of stars with and without planets. This result does not depend on either the planet mass, from 7 Earth masses to 17.4 Jupiter masses, or the orbital period of the planets, from 3 to 4300 days. In addition, we have derived the slope of the abundance ratios as a function of the condensation temperature for each star and again find similar distributions of the slopes for both stars with and without planets. In particular, the peaks of these two distributions are placed at a similar value but with opposite sign as that expected from a possible signature of terrestial planets. In particular, two of the planetary systems in this sample, containing each of them a Super-Earth like planet, show slope values very close to these peaks which may suggest that these abundance patterns are not related to the presence of terrestial planets.Comment: Accepted for publication in The Astrophysical Journa

La piramide del estilo de vida saludable para niños y adolescentes

Introduction: Increasing evidence demonstrates that risk factors for chronic diseases are established during childhood and adolescence. Consensus about the need to increase prevention efforts makes the adoption of a healthy lifestyle seem desirable from early childhood onwards. After reviewing educational tools for children and adolescents aimed at promoting a healthy lifestyle, it was recognized that there was a need to develop a simple educational tool specifically designed for these age groups. Methods: Development of the healthy lifestyle pyramid for children and adolescents. Results: We propose a three-dimensional, truncated and staggered pyramid with 4 faces and a base, which introduces a completely new concept that goes beyond other published pyramids. Each of the faces is oriented towards achieving a different goal. Two faces (faces 1 and 2) are formulated around achieving a goal on a daily basis (daily food intake, face 1, and daily activities, face 2). Face 3 is an adaptation of the traditional food guide pyramid, adapted to children’s energy, nutritional and hydration needs. Face 4 deals with both daily and life-long habits. On the base of the pyramid, there is advice about adequate nutrition alternating with advice about physical activity and sports. Conclusion: The Healthy Lifestyle Pyramid© is specifically developed for children and adolescents according to current scientific knowledge and evidence-based data and includes easy-to-follow advice and full colour pictures. Following these guidelines should improve health and reduce risk factors, promoting enjoyable and appropriate development towards adulthood.Introducción: En la actualidad, existe evidencia científica de que los factores de riesgo de enfermedades crónicas se establecen durante la infancia y la adolescencia. La adopción de un estilo de vida saludable parece deseable desde edades tempranas existiendo un consenso cada vez mayor hacia la prevención. Al revisar las herramientas educativas existentes para niños y adolescentes dirigidas a la mejora de la adquisición de un estilo de vida saludable, se advirtió de la necesidad de desarrollar un instrumento educativo desarrollado específicamente para estos grupos de edad. Métodos: Desarrollo de la pirámide de estilo de vida saludable para los niños y adolescentes. Resultados: Nuestra propuesta trata de una pirámide tridimensional con 4 caras y una base, truncada y escalonada, introduciendo un nuevo concepto que va más allá de lo publicado en otras pirámides. Cada una de las caras se orienta hacia la consecución de un objetivo. Las dos primeras caras (caras 1 y 2) se han formulado con el fin de lograr un objetivo sobre una base diaria (alimentación diaria, la cara 1, frente a las actividades diarias la cara 2). La Cara 3 es una adaptación de la tradicional pirámide de alimentos, adecuada a las necesidades de energía, nutrientes e hidratación de los niños. La Cara 4 muestra los hábitos de higiene y salud que se deben mantener durante toda la vida. En la base de la pirámide, se alternan mensajes sobre la nutrición adecuada con mensajes relacionados con la actividad física y el deporte. Conclusión: La Pirámide del Estilo de Vida Saludable© se ha desarrollado específicamente para niños y adolescentes, teniendo en cuenta los actuales conocimientos científicos. Incluye mensajes fáciles de entender e imágenes a todo color. El seguimiento de estas directrices debería contribuir a mejorar la salud y a la reducción de los factores de riesgo en la edad adulta, al tiempo que se divierten y crecen de una manera aconsejable.The pyramid has been edited with the support of Coca-Cola España. The pyramid can be downloaded at EXERNET (www.spanishexernet.com), supported by the Spanish Ministry of Education. Reproduction permitted with the citation of this article

New Indicators for AGN Power: The Correlation Between [O IV] lambda 25.89 micron and Hard X-ray Luminosity for Nearby Seyfert Galaxies

We have studied the relationship between the [O IV] lambda 25.89 micron emission line luminosities, obtained from Spitzer spectra, the X-ray continua in the 2-10 keV band, primarily from ASCA, and the 14-195 keV band obtained with the SWIFT/Burst Alert Telescope (BAT), for a sample of nearby (z < 0.08) Seyfert galaxies. For comparison, we have examined the relationship between the [O III] 5007, the 2-10 keV and the 14-195 keV luminosities for the same set of objects. We find that both the [O IV] and [O III] luminosities are well-correlated with the BAT luminosities. On the other hand, the [O III] luminosities are better-correlated with 2-10 keV luminosities than are those of [O IV]. When comparing [O IV] and [O III] luminosities for the different types of galaxies, we find that the Seyfert 2's have significantly lower [O III] to [O IV] ratios than the Seyfert 1's. We suggest that this is due to more reddening of the narrow line region (NLR) of the Seyfert 2's. Assuming Galactic dust to gas ratios, the average amount of extra reddening corresponds to a hydrogen column density of ~ few times 10^21 cm^-2, which is a small fraction of the X-ray absorbing columns in the Seyfert 2's. The combined effects of reddening and the X-ray absorption are the probable reason why the [O III] versus 2-10 keV correlation is better than the [O IV] versus 2-10 keV, since the [O IV] emission line is much less affected by extinction. Overall, we find the [O IV] to be an accurate and truly isotropic indicator of the power of the AGN. This suggests that it can be useful in deconvolving the contribution of the AGN and starburst to the spectrum of Compton-thick and/or X-ray weak sources.Comment: Accepted for publication in the Astrophysical Journal. 31 pages, 6 figures, 4 table

The radius and mass of the close solar twin 18 Sco derived from asteroseismology and interferometry

The growing interest in solar twins is motivated by the possibility of comparing them directly to the Sun. To carry on this kind of analysis, we need to know their physical characteristics with precision. Our first objective is to use asteroseismology and interferometry on the brightest of them: 18 Sco. We observed the star during 12 nights with HARPS for seismology and used the PAVO beam-combiner at CHARA for interferometry. An average large frequency separation $134.4\pm0.3$ $\mu$Hz and angular and linear radiuses of $0.6759 \pm 0.0062$ mas and $1.010\pm0.009$ R$_{\odot}$ were estimated. We used these values to derive the mass of the star, $1.02\pm0.03$ M$_{\odot}$.Comment: 5 pages, 5 figure

Single-phase shunt active power filter with UPS operation using a bidirectional Dc-Dc converter for energy storage interface

This paper presents a single-phase shunt active power filter (SAPF) with bidirectional dc-dc converter for uninterruptible power supply (UPS) operation. The proposed system comprises two power converters, namely a dc-ac converter to interface the power grid and a bidirectional isolated dc-dc converter connected to a battery pack, with both converters sharing the same dc-link. The arrangement of the converters allows the operation of the system in three different modes: (1) As SAPF, during normal operation; (2) As off-line UPS, in case of power grid outages; (3) As battery charging system, combined with the operation as SAPF. Simulation results of these three modes are presented in the paper to prove the operation feasibility of the proposed system. A reduced-scale prototype was developed, and the main parameters of the control stage, as well as the implemented control algorithms and power structure, are described in the paper. The experimental results obtained highlight the main benefits of the developed prototype.This work has been supported by COMPETE: POCI-01- 0145-FEDER-007043 and FCT – Fundação para a Ciência e Tecnologia within the Project Scope: UID/CEC/00319/2013. This work is financed by the ERDF – European Regional Development Fund through the Operational Programme for Competitiveness and Internationalisation COMPETE 2020 Programme, and by National Funds through the Portuguese funding agency, FCT Fundação para a Ciência e a Tecnologia, within project SAICTPAC/0004/2015 POCI 01 0145 FEDER 016434.info:eu-repo/semantics/publishedVersio

The Iberian Chain: tertiary inversion of a mesozoic intraplate basin

The Mesozoic Iberian basin developed inside the Iberian plate in the eastern end of the Tethys sea. As a result of the Tertiary convergence between the Iberian plate with the European and African plates, the Iberian basin was contractionally inverted, giving rise to the Iberian and Catalan Coastal chains and the surrounding Tertiary basins. The Bouguer anomaly map of the area shows that the Iberian Chain has crustal roots which would have produced during the Tertiary contractional period

OPserver: interactive online-computations of opacities and radiative accelerations

Codes to compute mean opacities and radiative accelerations for arbitrary chemical mixtures using the Opacity Project recently revised data have been restructured in a client--server architecture and transcribed as a subroutine library. This implementation increases efficiency in stellar modelling where element stratification due to diffusion processes is depth dependent, and thus requires repeated fast opacity reestimates. Three user modes are provided to fit different computing environments, namely a web browser, a local workstation and a distributed grid.Comment: 5 pages, 1 figur