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2023 Acuerdos transformativos CRUE This work was supported by Chair Against Stigma UCM-Grupo 5 (CE222103G5), Background: Stigma towards people with intellectual disability affects various aspects of their lives, including access to employment, housing, health and social care services. Furthermore, this stigma reduces their social opportunities and is even reflected in laws that diminish their autonomy. Due to the practical significance of this issue, the aim of this research is to explore for the first time the social stigma associated with intellectual disability in a representative sample of the Spanish population. Method: A cross-sectional quantitative descriptive study was conducted, involving a representative sample of the population (N = 2746). The study includes descriptive analyses and hierarchical regressions to examine various dimensions of stigma, such as attitudes, attributions, and intentions of social distance. Results: Medium levels of stigma are found regarding attitudes and attributions towards people with intellectual disability, while levels are medium-low concerning the intention of social distance. The most reliable indicators of stigma across its various dimensions encompass attitudes, attributions, and the intention of social distance. Factors that contribute to lower stigma include knowing someone with an intellectual disability, being willing to discuss intellectual disability with an acquaintance who has it and having a progressive political ideology. People with intellectual disability show more negative attributions towards themselves. Living with a person with an intellectual disability is another predictor of more stigmatising attitudes, but less intention of social distance. Results are mixed regarding age, gender, and educational level. Conclusion: Combating the stigmatisation of people with intellectual disabilities must include comprehensive actions to address attitudes, attributions and behavioural intentions. Public policies, such as national campaigns and programmes, should include contact with and open conversations about intellectual, Depto. de Personalidad, Evaluación y Psicología Clínica, Depto. de Psicobiología y Metodología en Ciencias del Comportamiento, Fac. de Psicología, TRUE, pub, APC financiada por la UCM

[Abstract] Previous studies from the Iberian Central System and other mountains of the Iberian Peninsula and Europe suggest that deglaciation in this area occurred at the end or immediately after the global Last Glacial Maximum (LGM, 26.5–19 ka). In this research, we investigate the timing and speed of deglaciation of the palaeoglacier in La Vega gorge (Iberian Central system) since the global LGM, dating the outer moraines, glacially polished bedrock and glaciofluvial deposits by means of in situ cosmogenic 10Be and optically stimulated luminescence. The results show that one intermediate arc located at the outer frontal moraine system has an age of ~21 ka, being consistent with the global LGM. Deglaciation began at ~21–19 ka, speeding up at ~19 ka. We estimate that around 4–5 km of the palaeoglacier receded in ~1–2 kyrs since ~19 ka, leaving La Vega gorge probably ice-free at ~18 ka. Therefore, our data confirm that deglaciation in Sierra de Gredos began at the end of the global LGM, characterised by a rapid and massive retreat of glaciers.

Right-sided heart failure and tricuspid regurgitation are common and strongly associated with poor quality of life and an increased risk of heart failure hospitalizations and death. While medical therapy for right-sided heart failure is limited, treatment options for tricuspid regurgitation include surgery and, based on recent developments, several transcatheter interventions. However, the patients who might benefit from tricuspid valve interventions are yet unknown, as is the ideal time for these treatments given the paucity of clinical evidence. In this context, it is crucial to elucidate aetiology and pathophysiological mechanisms leading to right-sided heart failure and tricuspid regurgitation in order to recognize when tricuspid regurgitation is a mere bystander and when it can cause or contribute to heart failure progression. Notably, early identification of right heart failure and tricuspid regurgitation may be crucial and optimal management requires knowledge about the different mechanisms and causes, clinical course and presentation, as well as possible treatment options. The aim of this clinical consensus statement is to summarize current knowledge about epidemiology, pathophysiology and treatment of tricuspid regurgitation in right-sided heart failure providing practical suggestions for patient identification and management.

Aims: We aim to compare the incidence and in-hospital outcomes of communityacquired pneumonia (CAP), ventilator-associated pneumonia (VAP) and nonventilator hospital-acquired pneumonia (NV-HAP) according to gender. Methods: This was a retrospective observational epidemiological study using the Spanish National Hospital Discharge Database for the years 2016 and 2017. Results: Of 277 785 hospital admissions, CAP was identified in 257 455 (41.04% females), VAP was identified in 3261 (30.42% females) and NV-HAP was identified in 17 069 (36.58% females). The incidence of all types of pneumonia was higher amongst males (CAP: incidence rate ratio [IRR] 1.05, 95% CI 1.03-1.06; VAP: IRR 1.36, 95% CI 1.26-1.46; and NV-HAP: IRR 1.16, 95% CI 1.14-1.18). The crude in-hospital mortality (IHM) rate for CAP was 11.44% in females and 11.80% in males (P = .005); for VAP IHM, the rate was approximately 35% in patients of both genders and for NV-HAP IHM, the rate was 23.97% for females and 26.40% for males (P < .001). After multivariable adjustment, in patients of both genders, older age and comorbidities were factors associated with IHM in the three types of pneumonia analysed. Female gender was a risk factor for IHM after VAP (OR 1.24; 95% CI 1.06-1.44), and no gender differences were found for CAP or NV-HAP. Conclusions: Our findings show a difference between females and males, with females presenting a lower incidence of all types of pneumonia. However, female gender was a risk factor for IHM after VAP., Unión Europea, Instituto de Salud Carlos III, Depto. de Salud Pública y Materno - Infantil, Fac. de Medicina, TRUE, pub

Background Several mechanisms have been proposed to explain why some platelets have a reduced response to aspirin (ASA). Among them, it was reported an increased circulating level of vitamin-D-binding protein (DBP). In addition, nitric oxide (NO) released from mononuclear cells was involved in the antiplatelet effects of ASA. The aim was to analyse the relationship between platelet response to ASA and both NO generation and vitamin-D-binding protein content in mononuclear cells. Materials and methods Mononuclear cells were obtained from patients with stable coronary artery disease that were divided by a platelet functionality test (PFA-100) as ASA-sensitive (n = 23) and ASA resistant (n = 27). Results Both the release of NO (determined by nitrite + nitrate concentration) and the expression of endothelial-type NO synthase (eNOS) were higher in mononuclear cells from ASA sensitive as compared with those from ASA-resistant patients. There was a positive correlation between either the release of NO and the expression of eNOS protein in mononuclear cells with the ability of ASA to inhibit platelet activity. DBP content in mononuclear cells was higher in ASA resistant than in ASA sensitive. The level of DBP content in mononuclear cells was negatively associated with the ability of ASA to inhibit platelets. However, in vitro experiments suggested that there was no association between DBP and NO production by mononuclear cells. Conclusions Mononuclear cells from patients with platelets with lower responsiveness to ASA showed a reduced ability to produce NO., Depto. de Salud Pública y Materno - Infantil, Fac. de Medicina, FALSE, pub

Stroke patients have a high risk of vascular recurrence. Biomarkers related to vascular recurrence, however, remain to be identified. The aim of the study was to identify, through proteomic analysis, plasma biomarkers associated with vascular recurrence within one year after the first ischemic stroke. This is a substudy (n = 134) of a large prospective multicenter study of post-stroke patients with an ischemic stroke. Plasma samples were obtained at inclusion. Among the identified proteins, only plasma levels of desmoplakin I were associated with protection against a new vascular event (Odds ratio: 0.64; 95% CI: 0.46-0.89; p = 0.009) after adjustment for hypercholesterolemia, statins and previous atherothrombotic stroke subtype. A greater number of patients without vascular recurrence had been treated with statins within three months of the recent ischemic stroke. Only patients who had been taking statins for 3 months after the ischemic stroke and did not suffer vascular recurrence over a follow-up year, have higher levels of desmoplakin I at the time of inclusion (Odds ratio 0.49; 95% CI: 0.28-0.86; p = 0.013). Increased desmoplakin I levels, determined within 1-3 months of the first ischemic stroke, could be a biomarker for statin responsiveness against a new vascular event in post-ischemic stroke patients taking statins early (1-3 months) after the ischemic stroke., Brystol-Myers Squibb, Fondo de Investigaciones de la Seguridad Social, Depto. de Salud Pública y Materno - Infantil, Fac. de Medicina, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2014 The Autors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. Meteor stations deployed at Sevilla, La Hita, Huelva, El Arenosillo, Sierra Nevada and La Pedriza have been funded by the first author. We acknowledge partial support from the Spanish Ministry of Science and Innovation (projects AYA2011-26522, AYA2012-31277 and AYA2012-30717). We thank the AstroHita Foundation for its continuous support in the operation of the meteor observing station located at La Hita Astronomical Observatory., We have analysed the meteor activity associated with meteoroids of fresh dust trails of Comet 209P/LINEAR, which produced an outburst of the Camelopardalid meteor shower (IAU code #451, CAM) in 2014 May. With this aim, we have employed an array of high-sensitivity CCD video devices and spectrographs deployed at 10 meteor observing stations in Spain in the framework of the Spanish Meteor Network. Additional meteoroid flux data were obtained by means of two forward-scatter radio systems. The observed peak zenithal hourly rate was much lower than expected, of around 20 meteors h(-1). Despite of the small meteor flux in the optical range, we have obtained precise atmospheric trajectory, radiant and orbital information for 11 meteor and fireball events associated with this stream. The ablation behaviour and low tensile strength calculated for these particles reveal that Camelopardalid meteoroids are very fragile, mostly pristine aggregates with strength similar to that of the Orionids and the Leonids. The mineral grains seem to be glued together by a volatile phase. We also present and discuss two unique emission spectra produced by two Camelopardalid bright meteors. These suggest a non-chondritic nature for these particles, which exhibit Fe depletion in their composition., Spanish Ministry of Science and Innovation, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2011 RAS. © The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. It is a pleasure to thank the many people who welcomed our project into the 3.5-m telescope in CAHA, where we always felt at home. We also thank the invaluable work of our anonymous referee, which greatly improved the quality of this manuscript. J. Pérez Gallego thanks Sun Mi Chung, Bruno Ferreira, Carlos Hoyos, Carlos Román and Sebastián Sánchez for their selfless help and interesting conversations throughout the development of the work presented in this paper. J. Pérez Gallego acknowledges support from a University of Florida Alumni Fellowship, and R. Guzman from NASA grant LTSA NA65-11635. This work is partially funded by the Spanish MICINN under the Consolider Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc/). This work is also partially funded by the Spanish Programa de Astronomía y Astrofísica under grants AYA2006-02358 and AYA2006-15698-C02-02., We use three-dimensional optical spectroscopy observations of a sample of 22 local luminous compact blue galaxies (LCBGs) to create kinematic maps. By means of these, we classify the kinematics of these galaxies into three different classes: rotating disc (RD), perturbed rotation (PR) and complex kinematics (CK). We find 48 per cent are RDs, 28 per cent are PRs and 24 per cent are CKs. RDs show rotational velocities that range between similar to 50 and similar to 200 km s(-1), and dynamical masses that range between similar to 1 x 10(9) and similar to 3 x 10(10) M(circle dot). We also address the following two fundamental questions through the study of the kinematic maps: (i) What processes are triggering the current starburst in LCBGs? We search our maps of the galaxy velocity fields for signatures of recent interactions and close companions that may be responsible for the enhanced star formation in our sample. We find that 5 per cent of objects show evidence of a recent major merger, 10 per cent of a minor merger and 45 per cent of a companion. This argues in favour of ongoing interactions with close companions as a mechanism for the enhanced star formation activity in these galaxies. (ii) What processes may eventually quench the current starbust in LCBGs? Velocity and velocity width maps, together with emission line ratio maps, can reveal signatures of active galactic nuclei (AGNs) activity or supernova (SN)-driven galactic winds that could halt the current burst. We find only 5 per cent of objects with clear evidence of AGN activity and 27 per cent with kinematics consistent with SN-driven galactic winds. Therefore, a different mechanism may be responsible for quenching the star formation in LCBGs. Finally, from our analysis, we find that the velocity widths of RDs, rather than accounting exclusively for the rotational nature of these objects, may account as well for other kinematic components and may not be good tracers of their dynamical masses., University of Florida, NASA, Spanish MICINN, Spanish Programa de Astronomía y Astrofísica, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

©Wiley & Sons. This paper is partially based on data from CAHA, the German-Spanish Astronomical Centre, Calar Alto, operated by the Max-Planck-Institute for Astronomy, Heidelberg, jointly with the Spanish National Commission for Astronomy. Also partially based on data obtained with the 2.3m Bok Telescope of the University of Arizona on Kitt Peak National Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc. (AURA) under cooperative agreement with the National Science Foundation. Also partially based on observations made with the Isaac Newton and Jacobus Kapteyn Telescopes, operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias. This research has made use of the NASA/IPAC Extragalactic Database (NED) and the NASA/IPAC Infrared Science Archive which are operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. PGPG wishes to acknowledge the Spanish Ministry of Education and Culture for the reception of a Formación de Profesorado Universitario fellowship. AGdP acknowledges financial support from NASA through a Long Term Space Astrophysics grant to B.F. Madore. During the course of this work AAH has been supported by the National Aeronautics and Space Administration grant NAG 5-3042 through the University of Arizona and Contract 960785 through the Jet Propulsion Laboratory. AAS acknowledges generous financial support from the Royal Society. We also would like to thank George and, We present an analysis of the integrated properties of the stellar populations in the Universidad Complutense de Madrid (UCM) Survey of Halpha-selected galaxies. In this paper, the first of a series, we describe in detail the techniques developed to model star-forming galaxies using a mixture of stellar populations, and taking into account the observational uncertainties. We assume a recent burst of star formation superimposed on a more evolved population. The effects of the nebular continuum, line emission and dust attenuation are taken into account. We also test different model assumptions, including the choice of specific evolutionary synthesis model, initial mass function, star formation scenario and the treatment of dust extinction. Quantitative tests are applied to determine how well these models fit our multiwavelength observations for the UCM sample. Our observations span the optical and near-infrared, including both photometric and spectroscopic data. Our results indicate that extinction plays a key role in this kind of study, revealing that low- and high-obscured objects may require very different extinction laws and must be treated differently. We also demonstrate that the UCM Survey galaxies are best described by a short burst of star formation occurring within a quiescent galaxy, rather than by continuous star formation. A detailed discussion on the inferred parameters, such as the age, burst strength, metallicity, star formation rate, extinction and total stellar mass for individual objects, is presented in Paper II of this series., National Aeronautics and Space Administration (NASA), National Science Foundation (NSF), EE.UU., Ministerio de Educación, Cultura y Deporte (MECD), España, University of Arizona, Jet Propulsion Laboratory, EE.UU., Royal Society, RU, Plan Nacional de Astronomía y Astrofísica (MICINN), España, Ministerio de ciencia e Innovación (MICINN), España, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2010 The Authors © 2010 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. We are grateful to the anonymous referee for his valuable comments which have led to an improvement in this paper. We acknowledge support from the Spanish Programa Nacional de Astronomía y Astrofísica under grants AYA2006-02358 and AYA2006-15698-C02-02. This work is partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC. ACM acknowledges support from the Juan de la Cierva Program financed by the Spanish MICINN. JPG acknowledges support from a University of Florida Alumni Fellowship and RG from NASA Grant LTSA NA65-11635. SFS thanks the sub-programs of Viabilidad, Diseño, Acceso y Mejora de ICTS ICTS-2009-10 and the PAI Proyecto de Excelencia P08-FWM-04319 and the funds of the PAI research group FQM360. SFS thanks the Spanish Plan Nacional de Astronomía program AYA2005-09413-C02-02., Physical properties of the star-forming regions in the local Luminous Compact Blue Galaxy (LCBG) NGC 7673 are studied in detail using 3D spectroscopic data taken with the PMAS fibre pack (PPAK) integral field unit at the 3.5-m telescope in the Centro Astronomico Hispano Aleman (CAHA). We derive integrated and spatially resolved properties such as extinction, star formation rate (SFR) and metallicity for this galaxy. Our data show an extinction map with maximum values located at the position of the main clumps of star formation showing small spatial variations [E(B - V)(t) = 0.12-0.21 mag]. We derive an H alpha-based SFR for this galaxy of 6.2 +/- 0.8M(circle dot) yr(-1) in agreement with the SFR derived from infrared and radio continuum fluxes. The star formation is located mainly in clumps A, B, C and F. Different properties measured in clump B make this region peculiar. We find the highest H alpha luminosity with an SFR surface density of 0.5 M-circle dot yr(-1) kpc(-2) in this clump. In our previous work, the kinematic analysis for this galaxy shows an asymmetrical ionized gas velocity field with a kinematic decoupled component located at the position of clump B. This region shows the absence of strong absorption features and the presence of a Wolf-Rayet stellar population indicating that this is a young burst of massive stars. Furthermore, we estimate a gas metallicity of 12 + log(O/H) = 8.20 +/- 0.15 (0.32 solar) for the integrated galaxy using the R23 index. The values derived for the different clumps with this method show small metallicity variations in this galaxy, with values in the range 8.12 (for clump A) to 8.23 (for clump B) for 12 + log(O/H). The analysis of the emission-line ratios discards the presence of any active galactic nuclei (AGN) activity or shocks as the ionization source in this galaxy. Between the possible mechanisms to explain the starburst activity in this galaxy, our 3D spectroscopic data support the scenario of an on-going interaction, Spanish Programa Nacional de Astronomía y Astrofísica, Spanish MICINN, University of Florida Alumni Fellowship, NASA, Viabilidad, Diseno, Acceso y Mejora de ICTS, PAI Proyecto de Excelencia, PAI, Spanish Plan Nacional de Astronomía, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub

This article has been accepted for publication in Monthly notices of the Royal Astronomical Society. © 2009 The Authors. Journal compilation © 2009 RAS. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved. It is a pleasure to thank those people who welcomed our project into the 3.5-m telescope in CAHA, where we always felt at home, especially those cozy snowy nights full of pastries and hot chocolates. We would especially like to thank Ana Guijarro, Jesús Aceituno and Santos Pedraz. We also thank Carlos Hoyos for interesting and highlighting discussions. Finally, we thank our referee, Matthew Bershady, for his helpful comments and suggestions. JPG acknowledges support from a University of Florida Alumni Fellowship and RG from NASA Grant LTSA NA65-11635. This work is partially funded by the Spanish MICINN under the Consolider-Ingenio 2010 Programme grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingenio-gtc). This work is partially funded by the Spanish Programa de Astronomía y Astrofísica under grants AYA2006-02358 and AYA2006-15698-C02-02., The kinematic properties of the ionized gas of local luminous compact blue galaxy NGC 7673 are presented using three-dimensional data taken with the PPAK integral field unit at the 3.5-m telescope in the Centro Astronomico Hispano Aleman. Our data reveal an asymmetric rotating velocity field with a peak-to-peak difference of 60 km s(-1). The kinematic centre is found to be at the position of a central velocity width maximum (sigma = 54 +/- 1 kms(-1)), which is consistent with the position of the luminosity-weighted centroid of the entire galaxy. The position angle of the minor rotation axis is 168 degrees as measured from the orientation of the velocity field contours. At least two decoupled kinematic components are found. The first one is compact and coincides with the position of the second most active star formation region (clump B). The second one is extended and does not have a clear optical counterpart. No evidence of active galactic nuclei activity or supernovae galactic winds powering any of these two components has been found. Our data, however, show evidence in support of a previously proposed minor merger scenario in which a dwarf galaxy, tentatively identified with clump B, is falling into NGC 7673 and triggers the starburst. Finally, it is shown that the dynamical mass of this galaxy may be severely underestimated when using the derived rotation curve or the integrated velocity width, under the assumption of virialization., University of Florida Alumni Fellowship, NASA, Spanish MICINN, Spanish Programa de Astronomia y Astrofisica, Depto. de Física de la Tierra y Astrofísica, Fac. de Ciencias Físicas, TRUE, pub