Suchergebnisse

The fight against private corruption is a highly complex criminal phenomenon that needs to be tackled by the European Union, by joint and uniform actions. For the Member States to face this social scourge en bloc, in an integrated manner, it is essential to achieve a proper understanding of the commercial bribery conduct that should be criminally relevant. To do this, we cannot avoid the controversial question relating to the criminal interest protected by this offence. For such purpose, we will examine the content of Council Framework Decision 2003/568/JHA, of 22 July 2003, and the status and new legislative tre nds concerning with the incriminating models implemented by France, Italy and Germany.Finally, we will conclude our study examining the latest developments in our country ; La lucha contra la corrupción privada, al tratarse de un fenómeno criminal de gran complejidad, requiere ser abordada por la Unión Europea de un modo conjunto y uniforme. Para que los Estados miembros puedan hacer frente en bloque a esta lacra social, de forma integrada, es esencial que exista una debida comprensión de las conductas de soborno comercial que deben ser penalmente relevantes, siendo de ineludible tratamiento la discutida cuestión del interés penalmente tutelado por este delito. A tal fin se examinará el contenido de la Decisión Marco 2003/568/JAI del Consejo, de 22 de julio de 2003, y el estado y nuevas tendencias legislativas de los modelos incriminatorios adoptados por Francia, Italia, Alemania, para finalizar con las últimas novedades habidas en nuestro país

The criminalization of the commercial bribery in the Código Orgánico Integral Penal (COIP) is part of an expansive and intensive current of criminal law that is not exclusive or autonomous for Ecuador. In the fresh anti-corruption legislation, several important issues can be observ ed, perhaps originated from the conflict that exists with the limiting principles of Criminal Law, within the constitutional system of rights and justice, as well as other unknowns when interpreting the objective elements of the offence, especially if we consider the criminal policy that seeks to satisfy this need. Applying an analytical and comparative methodology to these current issues, the Spanish experience in criminal matters can serve as a guide, since it incorporated a similar figure into its legislation more than a decade ago. From this perspective, some conclusions may be established that will emphasize the need to amend the Comprehensive Organic Criminal Code to prevent foreseeable problems in the application of the new offence. ; La criminalización de los actos de corrupción en el sector privado en el Código Orgánico Integral Penal (COIP) forma parte de una corriente expansiva e intensiva del Derecho penal que no es aislada o autónoma para el Ecuador. En la nueva legislación anticorrupción es posible observar ciertos problemas, tal vez derivados de los conflictos que existen con los principios limitadores del Derecho penal, dentro del modelo constitucional de derechos y justicia, así como otras incógnitas a la hora de interpretar los elementos objetivos del tipo penal, sobre todo si se tiene en cuenta la política criminal que busca satisfacer esta necesidad. Aplicando una metodología analítica y comparativa frente a estas actuales cuestiones, la experiencia española en materia penal puede servir de guía, por cuanto incorporó a su legislación una figura similar hace ya más de una década. Desde esta perspectiva podrán establecerse una serie de conclusiones que acentuarán la necesidad de reformar el Código Orgánico Integral ...

Although a catalogue of synthetic RGB magnitudes, providing photometric data for a sample of 1346 bright stars, has been recently published, its usefulness is still limited due to the small number of reference stars available, considering that they are distributed throughout the whole celestial sphere, and the fact that they are restricted to Johnson V < 6.6 mag. This work presents synthetic RGB magnitudes for ∼15 million stars brighter than Gaia G = 18 mag, making use of a calibration between the RGB magnitudes of the reference bright star sample and the corresponding high-quality photometric G, GBP, and GRP magnitudes provided by the Gaia EDR3. The calibration has been restricted to stars exhibiting -0.5 < GBP - GRP < 2.0 mag, and aims to predict RGB magnitudes within an error interval of ±0.1 mag. Since the reference bright star sample is dominated by nearby stars with slightly undersolar metallicity, systematic variations in the predictions are expected, as modelled with the help of stellar atmosphere models. These deviations are constrained to the ±0.1-mag interval when applying the calibration only to stars scarcely affected by interstellar extinction and with metallicity compatible with the median value for the bright star sample. The large number of Gaia sources available in each region of the sky should guarantee high-quality RGB photometric calibrations. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. ; The authors acknowledge financial support from the Spanish Programa Estatal de I+D + i Orientada a los Retos de la Sociedad under grant RTI2018-096188B-I00, which is partly funded by the European Regional Development Fund (ERDF), S2018/NMT-4291 (TEC2SPACE-CM), and ACTION, a project funded by the European Union H2020-SwafS-2018-1-824603. The participation of ICCUB researchers was (partially) supported by the Spanish Ministry of Science, Innovation and University (MICIU/FEDER, UE) through grant RTI2018095076-B-C21, and the Institute of Cosmos Sciences University of Barcelona (ICCUB, Unidad de Excelencia 'María de Maeztu') through grant CEX2019-000918-M. SB acknowledges Xunta de Galicia for financial support under grant ED431B 2020/29. The participation of ASdM was (partially) supported by the EMISSI@N project (NERC grant NE/P01156X/1). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. ; With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709. ; Peer reviewed

Although the use of RGB photometry has exploded in the last decades due to the advent of high-quality and inexpensive digital cameras equipped with Bayer-like colour filter systems, there is surprisingly no catalogue of bright stars that can be used for calibration purposes. Since due to their excessive brightness, accurate enough spectrophotometric measurements of bright stars typically cannot be performed with modern large telescopes, we have employed historical 13-colour medium-narrow-band photometric data, gathered with quite reliable photomultipliers, to fit the spectrum of 1346 bright stars using stellar atmosphere models. This not only constitutes a useful compilation of bright spectrophotometric standards well spread in the celestial sphere, the UCM library of spectrophotometric spectra, but allows the generation of a catalogue of reference RGB magnitudes, with typical random uncertainties ∼0.01 mag. For that purpose, we have defined a new set of spectral sensitivity curves, computed as the median of 28 sets of empirical sensitivity curves from the literature, that can be used to establish a standard RGB photometric system. Conversions between RGB magnitudes computed with any of these sets of empirical RGB curves and those determined with the new standard photometric system are provided. Even though particular RGB measurements from single cameras are not expected to provide extremely accurate photometric data, the repeatability and multiplicity of observations will allow access to a large amount of exploitable data in many astronomical fields, such as the detailed monitoring of light pollution and its impact on the night sky brightness, or the study of meteors, Solar system bodies, variable stars, and transient objects. In addition, the RGB magnitudes presented here make the sky an accessible and free laboratory for the calibration of the cameras themselves. © 2021 The Author(s). ; The authors acknowledge financial support from the Spanish Programa Estatal de I+D+i Orientada a los Retos de la Sociedad under grant RTI2018-096188-B-I00, which is partly funded by the European Regional Development Fund (ERDF), S2018/NMT-4291 (TEC2SPACE-CM), and ACTION, a project funded by the European Union H2020-SwafS-2018-1-824603. SB acknowledges Xunta de Galicia for financial support under grant ED431B 2020/29. The participation of ASdM was (partially) supported by the EMISSI@N project (NERC grant no. NE/P01156X/1). This work has been possible thanks to the extensive use of IPython and Jupyter notebooks (Pérez & Granger 2007). This research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013, 2018), NUMPY (Harris et al. 2020), SCIPY (Virtanen et al. 2020), and MATPLOTLIB (Hunter 2007). This research has made use of the Simbad data base and the VizieR catalogue access tool, CDS, Strasbourg, France (DOI:10.26093/cds/vizier). The original description of the VizieR service was published in A&AS, 143, 23. ; With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709. ; Peer reviewed