Innovación Docente en Historia Económica en el EEES

El Proyecto de Innovación Docente se aplicó sobre 450 alumnos de la asignatura de Historia Económica en el primer curso del Grado de Finanzas y Contabilidad. En esta asignatura se había utilizado tradicionalmente una metodología basada en clases magistrales con el apoyo de lecturas y materiales complementarios. El proyecto docente introducía una metodología de enseñanza mixta utilizando la plataforma virtual de la Universidad de Sevilla. A través de esta plataforma se realizaron actividades presenciales y también de e-learning en la web. La temática principal de estas actividades se centró en las crisis económicas. Esto se concretó a partir de estudio de casos: la crisis finisecular del siglo XIX, la crisis de 1929 y las crisis de finales del siglo XX y principios del XXI (crisis del petróleo de 1973, crisis financiera de los años 90 y la crisis económica actual). A través del material aportado por el profesor en la red y en las actividades complementarias presenciales (prensa, lecturas de historia económica y documentales) se establecen las causas, efectos y aspectos comunes y diferenciales de estas crisis.The Teaching Innovation Project was applied to 450 students of the Subject of Economic History of the first year of the Finance and Accounting Degree. This topic had used to be a traditional method based on master classes with the support of complementary readings and dossiers. Teaching project introduced a blended learning using the University of Seville web site. Through this platform and attending classes were also e-learning. The main topic of these activities are focused on the economic crisis with cases studies: the crisis of 1873, the Great Depression of 1929, the crisis of 1973 oil crisis, financial crisis 90’s years and the current economic crisis. Through the network materials, and exercises in class (press, reading of economic history and documentaries are established the causes, effects and common and differents aspects of these crisis

Gaia Data Release 1. Astrometry: one billion positions, two million proper motions and parallaxes

Context. Gaia Data Release 1 (DR1) contains astrometric results for more than 1 billion stars brighter than magnitude 20.7 based on observations collected by the Gaia satellite during the first 14 months of its operational phase. Aims. We give a brief overview of the astrometric content of the data release and of the model assumptions, data processing, and validation of the results. Methods. For stars in common with the Hipparcos and Tycho-2 catalogues, complete astrometric single-star solutions are obtained by incorporating positional information from the earlier catalogues. For other stars only their positions are obtained, essentially by neglecting their proper motions and parallaxes. The results are validated by an analysis of the residuals, through special validation runs, and by comparison with external data. Results. For about two million of the brighter stars (down to magnitude ∼11.5) we obtain positions, parallaxes, and proper motions to Hipparcos-type precision or better. For these stars, systematic errors depending for example on position and colour are at a level of ±0.3 milliarcsecond (mas). For the remaining stars we obtain positions at epoch J2015.0 accurate to ∼10 mas. Positions and proper motions are given in a reference frame that is aligned with the International Celestial Reference Frame (ICRF) to better than 0.1 mas at epoch J2015.0, and non-rotating with respect to ICRF to within 0.03 mas yr−1 . The Hipparcos reference frame is found to rotate with respect to the Gaia DR1 frame at a rate of 0.24 mas yr−1 . Conclusions. Based on less than a quarter of the nominal mission length and on very provisional and incomplete calibrations, the quality and completeness of the astrometric data in Gaia DR1 are far from what is expected for the final mission products. The present results nevertheless represent a huge improvement in the available fundamental stellar data and practical definition of the optical reference frame

Nuevo Portal Digital de Revistas Marcial Pons

Comunicación presentada en el 9º Workshop de Rebiun sobre proyectos digitales, Investigación, innovación e información: tendencias en los sistemas digitales de gestión de la producción científica, celebrado en Salamanca los días 1 y 2 de octubre de 2009.[ES] En esta presentación se lleva a cabo una explicación acerca del nuevo portal digital de revistas Pons en la que eplica la agencia de suscripciones del portal, el propio portal de revistas y la posibildad de acceso de los clientes.[EN] This presentation is carried out an explanation about the new digital portal Pons journal where subscriptions eplica agency portal, the portal itself posibildad magazines and customer access

Gaia Data Release 2 - The astrometric solution

Context. Gaia Data Release 2 (Gaia DR2) contains results for 1693 million sources in the magnitude range 3 to 21 based on observations collected by the European Space Agency Gaia satellite during the first 22 months of its operational phase. Aims. We describe the input data, models, and processing used for the astrometric content of Gaia DR2, and the validation of these results performed within the astrometry task. Methods. Some 320 billion centroid positions from the pre-processed astrometric CCD observations were used to estimate the five astrometric parameters (positions, parallaxes, and proper motions) for 1332 million sources, and approximate positions at the reference epoch J2015.5 for an additional 361 million mostly faint sources. These data were calculated in two steps. First, the satellite attitude and the astrometric calibration parameters of the CCDs were obtained in an astrometric global iterative solution for 16 million selected sources, using about 1% of the input data. This primary solution was tied to the extragalactic International Celestial Reference System (ICRS) by means of quasars. The resulting attitude and calibration were then used to calculate the astrometric parameters of all the sources. Special validation solutions were used to characterise the random and systematic errors in parallax and proper motion. Results. For the sources with five-parameter astrometric solutions, the median uncertainty in parallax and position at the reference epoch J2015.5 is about 0.04 mas for bright (G < 14 mag) sources, 0.1 mas at G = 17 mag, and 0.7 mas at G = 20 mag. In the proper motion components the corresponding uncertainties are 0.05, 0.2, and 1.2 mas yr 1, respectively. The optical reference frame defined by Gaia DR2 is aligned with ICRS and is non-rotating with respect to the quasars to within 0.15 mas yr 1. From the quasars and validation solutions we estimate that systematics in the parallaxes depending on position, magnitude, and colour are generally below 0.1 mas, but the parallaxes are on the whole too small by about 0.03 mas. Significant spatial correlations of up to 0.04 mas in parallax and 0.07 mas yr 1 in proper motion are seen on small (<1 deg) and intermediate (20 deg) angular scales. Important statistics and information for the users of the Gaia DR2 astrometry are given in the appendices

Gaia Data Release 1. Open cluster astrometry: performance, limitations, and future prospects

Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the astrometric data for open clusters. Methods. Mean cluster parallax and proper motion values are derived taking into account the error correlations within the astrometric solutions for individual stars, an estimate of the internal velocity dispersion in the cluster, and, where relevant, the e ects of the depth of the cluster along the line of sight. Internal consistency of the TGAS data is assessed. Results. Values given for standard uncertainties are still inaccurate and may lead to unrealistic unit-weight standard deviations of least squares solutions for cluster parameters. Reconstructed mean cluster parallax and proper motion values are generally in very good agreement with earlier Hipparcos-based determination, although the Gaia mean parallax for the Pleiades is a significant exception. We have no current explanation for that discrepancy. Most clusters are observed to extend to nearly 15 pc from the cluster centre, and it will be up to future Gaia releases to establish whether those potential cluster-member stars are still dynamically bound to the clusters. Conclusions. The Gaia DR1 provides the means to examine open clusters far beyond their more easily visible cores, and can provide membership assessments based on proper motions and parallaxes. A combined HR diagram shows the same features as observed before using the Hipparcos data, with clearly increased luminosities for older A and F dwarfs