¿Son bajos los flujos migratorios en España?

La Encuesta de Migraciones procedente de la EPA ha venido mostrando a lo largo del último decenio una baja y decreciente intensidad del flujo migratorio en España, incluso cuando nuestra economía ha atravesado etapas de recuperación y creación de empleo. Este sorprendente escenario que reflejan los datos se toma inverosímil cuando se comparan esas cifras con otras fuentes de información continua sobre la comente migratoria. Nuestro análisis de la metodología aplicada por el INE nos ha permitido establecer la existencia de una importante infravaloración congénita en la estimación de la movilidad a través de esta estadística.

Concept and measurement: the cultural borders of meaning

Paper submitted to the Sixth International Conference on Social Science Methodology, Amsterdam, The Netherlands, August 16-20, 2004.

Massive open star clusters using the VVV survey III. A young massive cluster at the far edge of the Galactic bar

Context. Young massive clusters are key to map the Milky Way’s structure, and near-infrared large area sky surveys have contributed strongly to the discovery of new obscured massive stellar clusters. Aims. We present the third article in a series of papers focused on young and massive clusters discovered in the VVV survey. This article is dedicated to the physical characterization of VVV CL086, using part of its OB-stellar population. Methods. We physically characterized the cluster using JHKS near-infrared photometry from ESO public survey VVV images, using the VVV-SkZ pipeline, and near-infrared K-band spectroscopy, following the methodology presented in the first article of the series. Results. Individual distances for two observed stars indicate that the cluster is located at the far edge of the Galactic bar. These stars, which are probable cluster members from the statistically field-star decontaminated CMD, have spectral types between O9 and B0 V. According to our analysis, this young cluster (1.0 Myr < age < 5.0 Myr) is located at a distance of 11+5-6 kpc, and we estimate a lower limit for the cluster total mass of (2.8+1.6-1.4) · 103 M⊙. It is likely that the cluster contains even earlier and more massive stars.