La divulgación de la Ciencia española en la Web 2.0: el caso del Consejo Superior de Investigaciones Científicas en Andalucía y Cataluña

El sistema ciencia, tecnología y sociedad no está consolidado en España por el desequilibrio que existe entre el desarrollo de la investigación y su divulgación. Además, la cultura científica de la sociedad está por debajo de la media europea y en la última década han descendido las vocaciones científicas entre los más jóvenes. En este contexto, se ha analizado si las instituciones de investigación utilizan las herramientas de la Web 2.0, principal canal de comunicación de los jóvenes entre 15 y 24 años, para mostrar a la sociedad los resultados de sus trabajos. Para ello, se han seleccionado como objeto de estudio los centros de investigación del Consejo Superior de Investigaciones Científicas en Andalucía y Cataluña. Entre los principales resultados obtenidos, a través del diseño de una checklist ad hoc, destaca el escaso uso que hacen de este canal de comunicación, ya que solo un 4,5% de los centros analizados utilizan todas las herramientas estudiadas. La efectividad de la comunicación ha sido otro de los valores observados, en este caso, en función de la conectividad (seguidores en sus perfiles sociales) e intensidad (número de publicaciones). Ambos ítems presentan también valores muy bajos. Por otro lado se observa un escaso nivel de popularidad de sus sitios web (número de enlaces que reciben) y una casi inexistente relación entre los mismos a través de hipervínculos que los conecten. Este último aspecto, se ha determinado con las herramientas webmétricas Webometric Analyst y ScoSciBot.

The Gaia-ESO Survey: processing FLAMES-UVES spectra

The Gaia-ESO Survey is a large public spectroscopic survey that aims to derive radial velocities and fundamental parameters of about 105 Milky Way stars in the field and in clusters. Observations are carried out with the multi-object optical spectrograph FLAMES, using simultaneously the medium-resolution (R ~ 20 000) GIRAFFE spectrograph and the high-resolution (R ~ 47 000) UVES spectrograph. In this paper we describe the methods and the software used for the data reduction, the derivation of the radial velocities, and the quality control of the FLAMES-UVES spectra. Data reduction has been performed using a workflow specifically developed for this project. This workflow runs the ESO public pipeline optimizing the data reduction for the Gaia-ESO Survey, automatically performs sky subtraction, barycentric correction and normalisation, and calculates radial velocities and a first guess of the rotational velocities. The quality control is performed using the output parameters from the ESO pipeline, by a visual inspection of the spectra and by the analysis of the signal-to-noise ratio of the spectra. Using the observations of the first 18 months, specifically targets observed multiple times at different epochs, stars observed with both GIRAFFE and UVES, and observations of radial velocity standards, we estimated the precision and the accuracy of the radial velocities. The statistical error on the radial velocities is σ ~ 0.4 km s-1 and is mainly due to uncertainties in the zero point of the wavelength calibration. However, we found a systematic bias with respect to the GIRAFFE spectra (~0.9 km s-1) and to the radial velocities of the standard stars (~0.5 km s-1) retrieved from the literature. This bias will be corrected in the future data releases, when a common zero point for all the set-ups and instruments used for the survey is be established.

The Gaia-ESO Survey: radial metallicity gradients and age-metallicity relation of stars in the Milky Way disk

We study the relationship between age, metallicity, and α-enhancement of FGK stars in the Galactic disk. The results are based upon the analysis of high-resolution UVES spectra from the Gaia-ESO large stellar survey. We explore the limitations of the observed dataset, i.e. the accuracy of stellar parameters and the selection effects that are caused by the photometric target preselection. We find that the colour and magnitude cuts in the survey suppress old metal-rich stars and young metal-poor stars. This suppression may be as high as 97% in some regions of the age-metallicity relationship. The dataset consists of 144 stars with a wide range of ages from 0.5 Gyr to 13.5 Gyr, Galactocentric distances from 6 kpcto 9.5 kpc, and vertical distances from the plane 0 < |Z| < 1.5 kpc. On this basis, we find that i) the observed age-metallicity relation is nearly flat in the range of ages between 0 Gyr and 8 Gyr; ii) at ages older than 9 Gyr, we see a decrease in [Fe/H] and a clear absence of metal-rich stars; this cannot be explained by the survey selection functions; iii) there is a significant scatter of [Fe/H] at any age; and iv) [Mg/Fe] increases with age, but the dispersion of [Mg/Fe] at ages >9 Gyr is not as small as advocated by some other studies. In agreement with earlier work, we find that radial abundance gradients change as a function of vertical distance from the plane. The [Mg/Fe] gradient steepens and becomes negative. In addition, we show that the inner disk is not only more α-rich compared to the outer disk, but also older, as traced independently by the ages and Mg abundances of stars.