Fluctuaciones de la extensión del casquete glacial de la isla Livingston (Shetland del Sur) desde 1956 hasta 1996

A partir de documentos cartográficos e imágenes de satélite se constata un 4,31% de reducción de extensión del casquete glacial de la isla Livingston desde 1956 hasta 1996. Se detecta la influencia de factores locales, fundamentalmente de tipo topogr á fico, que condicionan los avances y retrocesos del frente glacial en los diferentes sectores de la costa y se establece un modelo simple en el que se relaciona la reducción del conjunto del casquete con el calentamiento atmosférico experimentado en los últimos decenios en la zona de la Península Antártica.Cartographic data and satellite images have revealed that the area of the Livingston ice cap decreased by 4.31% from 1956 to 1996. Local factors, mainly topographic, have an influence on advances and retreats of the ice front. We established a simple model which correlates the reduction of the ice cap and the atmospheric wa rming detected in the Antarctic Peninsula during the last few decades

Fluctuaciones de la extensión del casquete glacial de la isla Livingston (Shetland del Sur) desde 1956 hasta 1996

Cartographic data and satellite images have revealed that the area of the Livingston ice cap decreased by 4.31% from 1956 to 1996. Local factors, mainly topographic, have an influence on advances and retreats of the ice front. We established a simple model which correlates the reduction of the ice cap and the atmospheric wa rming detected in the Antarctic Peninsula during the last few decades

Fotogrametría terrestre en el Glaciar Johnsons, Isla Livingston, Antártida

In order to apply precise cartography over areas where aerial photography is not available and classical topography is difficult or impossible, we propose photogrammetric techniques applied to terrestrial photography. In this paper we review the basic foundations of photogrammetry and the steps in the working methodology. We present application as example practical and compare the results to classical topographic measurements

Sal k 5, a member of the widespread Ole e 1-like protein family, is a new allergen of Russian thistle (Salsola kali) pollen.

Salsola kali is an Amaranthaceae weed with important repercussions for pollinosis in temperate areas. Ole e 1-like members are relevant allergens in pollen from different species. We aimed to characterize and produce as recombinant allergen S. kali Ole e 1-like protein. METHODS:The natural allergen was purified at homogeneity after three chromatographic steps. Specific cDNA was sequenced and expressed in Pichia pastoris yeast. Structural relationships of natural and recombinant forms were carried out by 2D electrophoresis and spectroscopic analyses. Its immunological relevance was analyzed by ELISA and immunoblotting using an IgG antiserum and monoclonal antibodies specific to Ole e 1, as well as sera from 57 allergic patients recruited from two Spanish regions where this pollinosis is frequent. RESULTS:The purified allergen, Sal k 5, is an acidic glycoprotein of 151 amino acid residues and 17,628 Da of molecular mass. Its amino acid sequence exhibits 68 and 32% identity with the allergens of Che a 1 and Ole e 1, respectively. The recombinant protein was correctly processed and its structural and immunologic equivalence to the natural form was proven. A sensitization frequency between 30 and 40% was observed in pollinic patients from the center and east coast of Spain. CONCLUSIONS:Sal k 5 is a member of the Ole e 1-like protein family which can be considered an important allergen from S. kali. Its inclusion in diagnosis protocols would allow the accurate defining of patients allergic to this pollen

Studying monogenetic volcanoes with a Terrestrial Laser Scanner: Case study at Croscat volcano (Garrotxa Volcanic Field, Spain)

Erosional processes (natural or anthropogenic) may partly destroy the relatively small-sized volcanic edifices characteristic of monogenetic volcanic zones, leaving their internal structure well exposed. Nevertheless, the study of these outcrops may be extremely challenging due to restricted accessibility or safety issues. Digital representations of the outcrop surface have been lately used to overcome such difficulties. Data acquired with terrestrial laser scanning instruments using Light Detection and Ranging technology enables the construction of such digital outcrops. The obtained high-precision 3-D terrain models are of greater coverage and accuracy than conventional methods and, when taken at different times, allow description of geological processes in time and space. Despite its intrinsic advantages and the proven satisfactory results, this technique has been little applied in volcanology-related studies. Here, we want to introduce it to the volcanological community together with a new and user-friendly digital outcrop analysis methodology for inexperienced users. This tool may be useful, not only for volcano monitoring purposes, but also to describe the internal structure of exposed volcanic edifices or to estimate outcrop erosion rates that may be helpful in terms of hazard assessment or preservation of volcanic landscapes. We apply it to the Croscat volcano, a monogenetic cone in the La Garrotxa Volcanic Field (Catalan Volcanic Zone, NE Spain), quarrying of which leads to a perfect view of its interior but restricts access to its uppermost parts. Croscat is additionally one of the most emblematic symbols of the La Garrotxa Volcanic Field Natural Park, and its preservation is a main target of the park administration

AISA Eagle II hyperspectral data for carbonate geological mapping in a vegetated high relief area: a geologically orientated atmospheric correction

[EN] Carbonated rocks are crucial targets for oil exploration, outcropping often in large areas with minimum spectral differences among geological units. The typical carbonate spectral absorptions in 2200 nm and 2300 nm, are excluded from the wavelength range of AISA Eagle II. AISA Eagle II hyperspectral data are processed in flight lines of 1024 swath pixels in the visible to near-infrared wavelength range (400 to 970 nm). The flight has a spatial resolution of 1 m and records a total of 128 channels with a spectral resolution of 4,8 nm. The area of study is a carbonate rocky mountain densely vegetated, covered by variably dense trees and bushes. Masking vegetation cover and shade effects is prior to any geological analysis using hyperspectral image processing. Carbonate units occur in mountain slopes, with small areas of ridges of rock outcrops and wide fans of loose material. The background soil of different geological units differ spectrally only by overall reflectance. Instead, limestone rocky outcrops display spectral responses with smooth typical iron oxide absorptions that distinguish them apart from loose boulders of limestone. Trying to enhance spectral differences in the visible wavelength range among carbonate geological units, an atmospheric correction using field spectra from geologically selected targets in a limestone quarry was performed. This way, it was possible to map apart lithologically similar detrital units dominated by carbonate in a river plain. The limy river bottom displays spectra with a straight line in the visible wavelength range due to abundant organic matter and small grain size. The spectra of the upper terraces record spectral absorption features related to iron oxide contents similar to the rock outcrops in ridges of mountains. The use of field spectra from geologically selected targets improves the mapping capability of hyperspectral imagery in areas with geological units with a homogeneous spectral response.[ES] Las calizas son rocas críticas en la exploración de petróleo. Desarrollan series estratigráficas a menudo espesas, que afloran con frecuencia en zonas extensas de la superficie terrestre. Estas formaciones litológicas predominantemente carbonatadas presentan diferencias espectrales mínimas entre sí, que permiten su diagnóstico por su respuesta espectral y su cartografía con imágenes. Las bandas de absorción espectral típicas de los carbonatos en 2200 nm y 2300 nm no forman parte del intervalo de longitudes de onda del espectrómetro AISA Eagle II (400 nm-970 nm), con una resolución espectral de 4,8 nm en 128 canales, y 1 m de resolución espacial en el vuelo de estudio. La zona de estudio se encuentra localizada en el Prepirineo español formando un relieve rocoso carbonatado con vegetación densa. El suelo de las distintas formaciones geológicas carbonatadas cartografiadas se distingue espectralmente sólo por su reflectancia global. Los afloramientos rocosos de calizas in situ presentan respuestas espectrales con absorciones típicas de óxidos de hierro. La expresión espectral de las formaciones calizas en las imágenes iniciales mostraban defectos sistemáticos. Para conseguir espectros geológicamente diagnosticables con espectrotecas de referencia, se ha ensayado una corrección atmosférica con espectros de campo tomados en una cantera de calizas, y en afloramientos rocosos de formaciones calcáreas seleccionados, con un espectrómetro de campo y laboratorio ASD Fieldspec 3. En las imágenes hiperespectrales así corregidas, se cartografían formaciones geológicas litológicamente similares correspondientes a la cuenca fluvial del río Noguera Ribagorzana, a su paso por Alfarrás (Lérida), en la que los sedimentos de la llanura aluvial con limos de materiales comparativamente más finos y materia orgánica, presentan espectros típicos con un trazo rectilíneo en el visible, que no aparecía en las imágenes anteriores a la corrección. El uso de espectros de campo seleccionados con criterios geológicos para la corrección atmosférica de imágenes hiperespectrales, mejora la capacidad de las imágenes para elaborar cartografías de formaciones litológicamente similares usando espectrotecas de referencia.El sensor AISA Eagle II fue cedido en préstamo por SPECIM al Institut Cartogràfic i Geològic de Catalunya (ICGC) para su prueba en vuelo y pre-tratamiento digital. Los estudios de interpretación geológica se han realizado en un convenio entre la Universidad de Barcelona y REPSOL Exploración para formación postdoctoral. Las bases para comenzar este trabajo surgieron durante la tesis doctoral de Buzzi (BES-2008-003648).Buzzi, J.; Costa, E.; Riaza, A.; Fernández, O.; García-Sellés, D.; Corbera, J. (2018). Cartografía de calizas con datos hiperespectrales AISA Eagle II en una zona montañosa con vegetación densa: cómo orientar geológicamente la corrección atmosférica. Revista de Teledetección. (51):125-133. https://doi.org/10.4995/raet.2018.8998SWORD12513351ASD. 2006. FieldSpecR 3 User Manual, ASD Document 600540 Rev. F. Analytical Spectral Devices, Inc. Disponible en: http://www.asdi.com [Último acceso: junio de 2018].Buzzi, J. 2012. Imaging spectroscopy to evaluate the contamination from sulphide mine waste in the Iberian Pyrite Belt using hyperspectral sensors (Huelva, Spain), Tesis Doctoral Universidad de León, 212 p.Buzzi, J., Riaza, A., García-Meléndez, Carrère, V., Bachmann, M. 2011. Aplicación de modelos Gaussianos modificados a datos hiperespectrales de una zona contaminada por drenaje ácido. Caso del río Odiel (Huelva, España). XIV Congreso de la Asociación Española de Teledetección, Mieres, 21- 23 Septiembre 2011, 285-288.Clark, R.N., Swayze, G.E., Wise, R., Livo, E., Hoefen, T., Kokaly, R., Sutley, S.J. 2007. USGS Digital Spectral Library splib06a. Digital Data Series 231, USGS: Denver, Co, USA, 2007.EXELIS, 2011. ENVI User's Guide. Exelis Visual Information Solutions: Boulder, Co, USA.Hunt, G.R., Salisbury, J.W. 1971a. Visible and Near-infrared Spectra of Minerals and Rocks: II. Carbonates. Modern Geology, 2, 23-30.Hunt, G.R., Salisbury, J.W., Lenhof, J. 1971b. Visible and Near-infrared Spectra of Minerals and Rocks: III Oxides and Hydroxides. Modern Geology, 2, 191-205.Hunt, G.R., Salisbury, J.W., 1976. Visible and Near-infrared Spectra of Minerals and Rocks: XI. Sedimentary Rocks. Modern Geology, 5, 211-217.López-Mir, B., Antón Muñoz, J., García-Senz, J. 2016, 3D geometric reconstruction of Upper Cretaceous passive diapirs and salt withdrawal basins in the Cotiella Basin (southern Pyrinees), Journal of the Geological Society, 173, 616-627. https://doi.org/10.1144/jgs2016-002Martínez, L., Tardà, A., Palà, V., Arbiol, R. 2006. Atmospheric correction algorithm applied to CASI multi-height hyperspectral imagery. Proceedings Second International Symposium Recent Advances in Quantitative Remote Sensing, 25-29 Septiembre 2006.Riaza, A. Buzzi, J., García-Meléndez, E., del Moral, B., Carrère, V., Richter, R. 2017. Monitoring salt crusts on an AMD contaminated coastal wetland using hyperspectral Hyperion data (Estuary of the River Odiel, SW Spain). International Journal of Remote Sensing, 38(12), 3735-3762. https://doi.org/10.1080/01431161.2017.1302621Riaza, A., García-Meléndez, E., Carrère, V., Mueller, A. 2014. Cartografía de sales marinas y fluviales en estuarios receptores de aguas ácidas con imágenes hiperespectrales Hyperion (Marismas del río Odiel, Huelva). Revista de Teledetección, 41, 1-7. https://doi.org/10.4995/raet.2014.2255Riaza, A., Buzzi, J., García-Meléndez, E., Carrère, V., Müller, A. 2011. Monitoring the extent of contamination from acid mine drainage in the Iberian Pyrite Belt (SW Spain) using hyperspectral imagery. Remote Sensing, 3, 2166-2186. https://doi.org/10.3390/rs3102166Riaza, A., Buzzi, J., García-Meléndez, E., Vázquez, I., Bellido, E., Carrère, V., Müller, A. 2012. Pyrite mine waste and water mapping using Hymap and Hyperion hyperspectral data. Environmental Earth Sciences, 66-7, 1957-1971. https://doi.org/10.1007/s12665-011-1422-

A 3-Biomarker 2-Point-Based Risk Stratification Strategy in Acute Heart Failure

Altres ajuts: ISCIII/RD06-0003-0000Altres ajuts: ISCIII/RD12/0042/0002Introduction and Objectives: Most multi-biomarker strategies in acute heart failure (HF) have only measured biomarkers in a single-point time. This study aimed to evaluate the prognostic yielding of NT-proBNP, hsTnT, Cys-C, hs-CRP, GDF15, and GAL-3 in HF patients both at admission and discharge. Methods: We included 830 patients enrolled consecutively in a prospective multicenter registry. Primary outcome was 12-month mortality. The gain in the C-index, calibration, net reclassification improvement (NRI), and integrated discrimination improvement (IDI) was calculated after adding each individual biomarker value or their combination on top of the best clinical model developed in this study (C-index 0.752, 0.715-0.789) and also on top of 4 currently used scores (MAGGIC, GWTG-HF, Redin-SCORE, BCN-bioHF). Results: After 12-month, death occurred in 154 (18.5%) cases. On top of the best clinical model, the addition of NT-proBNP, hs-CRP, and GDF-15 above the respective cutoff point at admission and discharge and their delta during compensation improved the C-index to 0.782 (0.747-0.817), IDI by 5% (p < 0.001), and NRI by 57% (p < 0.001) for 12-month mortality. A 4-risk grading categories for 12-month mortality (11.7, 19.2, 26.7, and 39.4%, respectively; p < 0.001) were obtained using combination of these biomarkers. Conclusion: A model including NT-proBNP, hs-CRP, and GDF-15 measured at admission and discharge afforded a mortality risk prediction greater than our clinical model and also better than the most currently used scores. In addition, this 3-biomarker panel defined 4-risk categories for 12-month mortality

<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

Role of age and comorbidities in mortality of patients with infective endocarditis

Purpose: The aim of this study was to analyse the characteristics of patients with IE in three groups of age and to assess the ability of age and the Charlson Comorbidity Index (CCI) to predict mortality. Methods: Prospective cohort study of all patients with IE included in the GAMES Spanish database between 2008 and 2015. Patients were stratified into three age groups:<65 years, 65 to 80 years, and = 80 years.The area under the receiver-operating characteristic (AUROC) curve was calculated to quantify the diagnostic accuracy of the CCI to predict mortality risk. Results: A total of 3120 patients with IE (1327 < 65 years;1291 65-80 years;502 = 80 years) were enrolled.Fever and heart failure were the most common presentations of IE, with no differences among age groups.Patients =80 years who underwent surgery were significantly lower compared with other age groups (14.3%, 65 years; 20.5%, 65-79 years; 31.3%, =80 years). In-hospital mortality was lower in the <65-year group (20.3%, <65 years;30.1%, 65-79 years;34.7%, =80 years;p < 0.001) as well as 1-year mortality (3.2%, <65 years; 5.5%, 65-80 years;7.6%, =80 years; p = 0.003).Independent predictors of mortality were age = 80 years (hazard ratio [HR]:2.78;95% confidence interval [CI]:2.32–3.34), CCI = 3 (HR:1.62; 95% CI:1.39–1.88), and non-performed surgery (HR:1.64;95% CI:11.16–1.58).When the three age groups were compared, the AUROC curve for CCI was significantly larger for patients aged <65 years(p < 0.001) for both in-hospital and 1-year mortality. Conclusion: There were no differences in the clinical presentation of IE between the groups. Age = 80 years, high comorbidity (measured by CCI), and non-performance of surgery were independent predictors of mortality in patients with IE.CCI could help to identify those patients with IE and surgical indication who present a lower risk of in-hospital and 1-year mortality after surgery, especially in the <65-year group

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