Efficacy and Feasibility of an Osteopathic Intervention for Neurocognitive and Behavioral Symptoms Usually Associated With Fetal Alcohol Spectrum Disorder.

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Remote sensing mediante LIDAR en la UPC

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Propuesta de mejora del Sistema Interno de Garantía de Calidad de la Facultad de Medicina

La garantía de calidad en el ámbito universitario puede considerarse como la atención sistemática, estructurada y continua a las titulaciones ofertadas. La garantía de calidad se compromete a poner en marcha los medios que aseguren y demuestren la calidad de los programas formativos que se desarrollan en cada una de las titulaciones ofrecidas por la Universidad y así cumplir con la obligación que tiene con la sociedad. El presente proyecto nace como fruto de la responsabilidad adquirida para el cumplimiento de las funciones encomendadas y, con el objetivo de seguir adoptando una estrategia de mejora continua de la calidad de la docencia y satisfacción de los colectivos implicados en el proceso de enseñanza-aprendizaje (Profesorado, Estudiantes y PAS)

<i>Gaia</i> Data Release 1. Summary of the astrometric, photometric, and survey properties

Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. Aims. A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. Methods. The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue. Results. Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the HIPPARCOS and Tycho-2 catalogues – a realisation of the Tycho-Gaia Astrometric Solution (TGAS) – and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of ∼3000 Cepheid and RR-Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yr−1 for the proper motions. A systematic component of ∼0.3 mas should be added to the parallax uncertainties. For the subset of ∼94 000 HIPPARCOS stars in the primary data set, the proper motions are much more precise at about 0.06 mas yr−1. For the secondary astrometric data set, the typical uncertainty of the positions is ∼10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to ∼0.03 mag over the magnitude range 5 to 20.7. Conclusions. Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data

Gaia Data Release 1: Testing parallaxes with local Cepheids and RR Lyrae stars

Context. Parallaxes for 331 classical Cepheids, 31 Type II Cepheids, and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). Aims. In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, which involve astrometry collected by Gaia during the initial 14 months of science operation, we compared them with literature estimates and derived new period-luminosity (PL), period-Wesenheit (PW) relations for classical and Type II Cepheids and infrared PL, PL-metallicity (PLZ), and optical luminosity-metallicity (M V -[Fe/H]) relations for the RR Lyrae stars, with zero points based on TGAS. Methods. Classical Cepheids were carefully selected in order to discard known or suspected binary systems. The final sample comprises 102 fundamental mode pulsators with periods ranging from 1.68 to 51.66 days (of which 33 with σ Ω /Ω < 0.5). The Type II Cepheids include a total of 26 W Virginis and BL Herculis stars spanning the period range from 1.16 to 30.00 days (of which only 7 with σ Ω /Ω < 0.5). The RR Lyrae stars include 200 sources with pulsation period ranging from 0.27 to 0.80 days (of which 112 with σ Ω /Ω < 0.5). The new relations were computed using multi-band (V,I,J,K s ) photometry and spectroscopic metal abundances available in the literature, and by applying three alternative approaches: (i) linear least-squares fitting of the absolute magnitudes inferred from direct transformation of the TGAS parallaxes; (ii) adopting astrometry-based luminosities; and (iii) using a Bayesian fitting approach. The last two methods work in parallax space where parallaxes are used directly, thus maintaining symmetrical errors and allowing negative parallaxes to be used. The TGAS-based PL,PW,PLZ, and M V - [Fe/H] relations are discussed by comparing the distance to the Large Magellanic Cloud provided by different types of pulsating stars and alternative fitting methods. Results. Good agreement is found from direct comparison of the parallaxes of RR Lyrae stars for which both TGAS and HST measurements are available. Similarly, very good agreement is found between the TGAS values and the parallaxes inferred from the absolute magnitudes of Cepheids and RR Lyrae stars analysed with the Baade-Wesselink method. TGAS values also compare favourably with the parallaxes inferred by theoretical model fitting of the multi-band light curves for two of the three classical Cepheids and one RR Lyrae star, which were analysed with this technique in our samples. The K-band PL relations show the significant improvement of the TGAS parallaxes for Cepheids and RR Lyrae stars with respect to the Hipparcos measurements. This is particularly true for the RR Lyrae stars for which improvement in quality and statistics is impressive. Conclusions. TGAS parallaxes bring a significant added value to the previous Hipparcos estimates. The relations presented in this paper represent the first Gaia-calibrated relations and form a work-in-progress milestone report in the wait for Gaia-only parallaxes of which a first solution will become available with Gaia Data Release 2 (DR2) in 2018. © ESO, 2017

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 effects 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

The Gaia mission

Gaia is a cornerstone mission in the science programme of the EuropeanSpace Agency (ESA). The spacecraft construction was approved in 2006, following a study in which the original interferometric concept was changed to a direct-imaging approach. Both the spacecraft and the payload were built by European industry. The involvement of the scientific community focusses on data processing for which the international Gaia Data Processing and Analysis Consortium (DPAC) was selected in 2007. Gaia was launched on 19 December 2013 and arrived at its operating point, the second Lagrange point of the Sun-Earth-Moon system, a few weeks later. The commissioning of the spacecraft and payload was completed on 19 July 2014. The nominal five-year mission started with four weeks of special, ecliptic-pole scanning and subsequently transferred into full-sky scanning mode. We recall the scientific goals of Gaia and give a description of the as-built spacecraft that is currently (mid-2016) being operated to achieve these goals. We pay special attention to the payload module, the performance of which is closely related to the scientific performance of the mission. We provide a summary of the commissioning activities and findings, followed by a description of the routine operational mode. We summarise scientific performance estimates on the basis of in-orbit operations. Several intermediate Gaia data releases are planned and the data can be retrieved from the Gaia Archive, which is available through the Gaia home page. http://www.cosmos.esa.int/gai

Sistema láser de medida de velocidad por efecto doppler de bajo coste para aplicaciones industriales e hidrodinámicas

La utilización práctica del efecto Doppler en la emisión láser fue propuesta desde los inicios del desarrollo de los láseres en los años sesenta. Sólo en los años ochenta la investigación realizada pudo salir del laboratorio y dar lugar a la fabricación de aparatos de medida de velocidad comerciales. A partir de los noventa estos aparatos se popularizaron rápidamente. Actualmente se utilizan medidores de velocidad láser por efecto Doppler en múltiples aplicaciones, entre las que sobresale la medida de velocidad de fluidos, para estudios aéreo e hidrodinámicos. Sus características únicas, como la precisión obtenida en la medida, su alta resolución espacial y el carácter no intrusivo, sólo han comenzado recientemente a tener rivales de consideración, como pueden ser la velocimetría de imagen de partículas (PIV). También la medida de velocidades de móviles sólidos comienza a resultar, con el abaratamiento general de los componentes opto-electrónicos, un objetivo para muchas empresas. Entre las aplicaciones de este tipo se contemplan el control de velocidad de los vehículos en carretera y el control de procesos industriales del ramo textil, papelero y deempresas fabricantes de cables, entre otros. Empresas europeas y americanas, como Dantec Electronik y TSI, por citar las más representativas, comercializan aparatos LDA de propósito general de altas prestaciones. Hasta la fecha estos sistemas sólo podían ser adquiridos por importantes centros de investigación o grandes empresas, debido a su elevado coste. El futuro comercial de la velocimetría láser Doppler exige la fabricación de aparatos más económicos y adaptados a las necesidades del cliente. Muchos de los sistemas actuales son voluminosos,difíciles de manejar y con potencias de trabajo elevadas. Se está llevando a cabo un importante trabajo para conseguir reducir el tamaño y coste de los equipos sin perder sus principales prestaciones. Asimismo la alta velocidad y capacidad de cálculo de los ordenadores personales actuales debe hacer innecesaria la inclusión de procesadores específicos para estos equipos.Presentamos el diseño y construcción de un sistema integral de medida de dos componentes de la velocidad, sistema 2D-LDA, para aplicaciones industriales e hidrodinámicas de baja potencia. Siguiendo la filosofía delineada arriba, el diseño de nuestro sistema LDA fue realizado utilizando únicamente una fuente laser y un módulo detector. Los sistemas LDA de medida de dos componentes de velocidad comercialmente disponibles, por el contrario, emplean dos longitudes de onda óptica y dos fotodetectores independientes. Las emisiones azul y verde típicas de los láseres de ion-Ar son las longitudes de onda a menudo elegidas en este tipo de medidas. Por otra parte, se ha empleado los dos canales de entrada de una tarjeta de adquisición de uso general para realizar el disparo multinivel. Esta configuración permite trabajar en cada momento con la parte de señal burst teóricamente más adecuada, con mayor valor de relación señal a ruido.Este trabajo ha sido financiado por la CICYT Proyecto PETRI 95-0249-OP:REALIZACIÓN DE SISTEMAS LÁSER PORTÁTILES DE MEDIDA DE VELOCIDAD POR EFECTO DOPPLER (LDA-LDV) DE BAJO COSTE PARA APLICACIONES INDUSTRIALES E HIDRODINÁMICAS.The practical use of the Doppler effect at optical wavelengths was proposed at the early beginning of the development of the laser, in the sixties. However, it was only in the eighties when the results of the experimental work could finally get out of the laboratories, and the first Laser Velocimeters were commercially available. In the nineties this kind of systems became rapidly popular. Nowadays the Laser Velocimeters based on the Doppler frequency shift find a lot of important applications, especially in some industrial processes and in hydrodynamic and aerodynamic research.The unique characteristics of the Laser Doppler Velocimetry (LDV) only recently have encountered a rival technique in the Particle Image Velocimetry (PIV), for applications on fluids. The main features of LDV systems are the accuracy and the speed of the measurements, the high spatial resolution and, of course, the non-intrusive character of the technique. Moreover this kind of systems present advantages not only in fluid applications: actually it can compete with the microwave radar in the estimation of the velocity of solid targets. This becomes possible due to theprogressive reduction of prices of optoelectronic devices and the improvement of its performances. The monitoring of the traffic velocity and the control of machinery in the manufacture of paper, wires and cables or thread can be mentioned among these applications.European an American companies, as Dantek Electronic or TSI, to mention the two most representative, commercialize high performance general-purpose LDV systems. Up to the date these instruments are sizeable and expensive, and its use requires some special training. There is not doubt that the future market of the LDV systems goes through a substantial decrease of prices and, indeed, through the possibility of custom-built designs. The potential number of users would increase then in an important manner. Many efforts are now being devoted by researchers in that direction. Moreover, the important improvement of capabilities of the desktop computers makes unnecessary the special electronic processors that, up to now, have been provided by the manufacturers of LDV systems as a part of them.In this Thesis the design and realization of a complete Laser Doppler Anemometer is presented. The system can measure two components of a fluid velocity (2D-LDA) and originally it was conceived to be used in industrial and hydrodynamics applications.Following the philosophy outlined above, the design of our LDA system was performed with only one laser source and one detector module. The common commercially available LDAs, on the contrary, designed to measure two components of velocity, use two different optical wavelengths and two independent photodiodes.On the other hand, a general-purpose acquisition card with two input channels has been used to implement a multilevel trigger. The configuration performed here permits to work in each moment with the part of the burst having the best signal to noise ratio.This work has been supported by the Spanish Government, CICYT project PETRI 95-0249-OP

Sedimentology, physical properties and age of mass transport deposits associated with the Marqués de Pombal Fault, Southwest Portuguese Margin

10 pages, 6 figures, 1 tableThe SW Iberian Margin is located at the convergence of the European and African Plates, where the largest magnitude earthquakes in Western Europe occur. Several active structures, such as the Marquês de Pombal fault, are potential sources of large magnitude earthquakes and tsunamis. Associated with faulting, submarine landslides are also commonly observed. A large area (~260 km2) of high acoustic backscatter in the central part of the Marquês de Pombal escarpment corresponds to a complex translational slide and debris flow. Detailed lithological description, physical properties and dating of four sediment cores sampled on the toe of the slide allow us to investigate the sediment facies, age and triggering mechanism of the Marquês de Pombal slides. The maximum age of the Marquês de Pombal landslide is 3270 ± 60 Cal yr BP. Radiocarbon dating of previous and subsequent Holocene mass wasting deposits gives an estimated recurrence rate of < 2 kyr. Although a number of mechanisms may be invoked to account for landslide triggering, earthquakes are the most likely triggering mechanism for the observed slope instabilities in the Marquês de Pombal area, at least during the HoloceneThe authors acknowledge the support of the MCYT Acción Especial HITS (REN2000-2150-E), Spanish national Project IMPULS (REN2003-05996MAR) and EUROMARGINS program of the European Science Foundation SWIM project (01-LEGEMA09F and REN2002-11234E-MAR)Peer Reviewe