Efectividad de un audiovisual como preparación para la cirugía en pacientes pediátricos

Las investigaciones sobre los pacientes pediátricos quirúrgicos, ponen en evidencia la urgente necesidad de preparlos psicológicamente para la hospitalización y la intervención. A este respecto, estudios realizados fuera de nuestro país han demostrado que la visualización de un audiovisual acerca de la hospitalización y el proceso quirúrgico es una técnica eficaz para ayudar a los niños y a sus progenitores a afrontar dicha situación. El objetivo del presente trabajo ha consistido en comprobar la eficacia de esta técnica en nuestro contexto hospitalario. Los resultados indican que la proyección de un audiovisual antes de la hospitalización es muy recomendable, dado que: 1) aclara dudas; 2) da una imagen más familiar del hospital; 3) estimula a los padres a hablar con sus hijos y 4) aumenta la satisfacción de los padres respecto a la información. Uno de los datos obtenidos que mayor refleja la eficacia del audiovisual es que el 98.2% de los padres recomendaría la visualización del audiovisual a otras familias.Research on paediatric surgical patients points to the urgent need to prepare them psychologically for hospitalisation and surgery. In this respect, studies conducted outside Spain have shown that seeing a video on hospitalisation and procedures for surgery is an effective technique for helping children and their parents to deal with this situation. The aim of the present work was to verify the effectiveness of this technique within the context of our hospitals. The results indicate that it is highly advisable to show such a video to patients and their parents before admission to hospital, since this: 1) clears up any doubts they might have; 2) gives a friendlier image of the hospitil; 3) encourages parents to talk to their children and 4) increases satisfaction among parents concerning the information they receive. One of the dadta which most clearly reflects the effectiveness of using the type of the audiovisual described is that 98.2% of parents would recommend other families to see it

Eficacia de una técnica cognitivo-conductual en pacientes quirúrgicos

El objetivo del estudio consistió en diseñar y comprobar la eficacia de una técnica psicológica en pacientes quirúrgicos, para reducir los niveles de ansiedad y depresión, y facilitar la recuperación. La muestra estuvo compuesta por 30 mujeres que debían someterse a una histerectomía abdominal. Estas mujeres fueron repartidas al azar en dos grupos: experimental y control. La técnica se compuso de diferentes elementos: 1) información; 2) expresión de emociones; 3) respiración, relajación, visualización; 4) ejercicios para facilitar la recuperación; 5) entrega de hojas informativas. Los resultados fueron: el grupo experimental respecto al grupo control, padeció menos ansiedad y depresión postquirúrgicas, sufrió menos dolor y complicaciones después de la operación, necesitó menos analgésicos, recuperó antes sus funciones orgánicas, y se acortó su estancia hospitalaria. Por tanto podemos concluir que la técnica psicológica diseñada se mostró eficaz como facilitadora de la recuperación en pacientes quirúrgicos.The aim of this study was to design and test the efficiency of a psychological technique to reduce levels of anxiety and depression in surgery patients and to facilitate their recovery. The test group was composed of 30 women who were to have a hysterectomy. These women were divided into two groups: an experimental group and a control group . The technique involved various elements: 1) information, 2) the expression of emotions, 3) breathing, relaxation, visualitation, 4) excercises to facilitate recovery, 5) distribution of summary sheets. The results were as follows: compared to the control group, the experimental group suffered less anxiety, less post-surgical depression, less pain and fewer post-operative complications. The women needed fewer painkillers, regained their normal bodily functions and needed a shorter stay in hospital. We can thus conclude that the psychological technique designed, proved efficient in facilitating the recovery of surgical patients

Evidence for intermediate-age stellar populations in early-type galaxies from K-band spectroscopy

The study of stellar populations in early-type galaxies in different environments is a powerful tool for constraining their star formation histories. This study has been traditionally restricted to the optical range, where dwarfs around the turn-off and stars at the base of the RGB dominate the integrated light at all ages. The near-infrared spectral range is especially interesting since in the presence of an intermediate-age population, AGB stars are the main contributors. In this letter, we measure the near-infrared indices NaI and D$_{\rm CO}$ for a sample of 12 early-type galaxies in low density environments and compare them with the Fornax galaxy sample presented by Silva et al. (2008). The analysis of these indices in combination with Lick/IDS indices in the optical range reveals i) the NaI index is a metallicity indicator as good as C4668 in the optical range, and ii) D$_{\rm CO}$ is a tracer of intermediate-age stellar populations. We find that low-mass galaxies in low density environments show higher NaI and D$_{\rm CO}$ than those located in Fornax cluster, which points towards a late stage of star formation for the galaxies in less dense environments, in agreement with results from other studies using independent methods.Comment: 7 pages, 3 figures, accepted for publication in ApJ

Non-parametric analysis of the rest-frame UV sizes and morphological disturbance amongst L* galaxies at 4<z<8

We present the results of a study investigating the sizes and morphologies of redshift 4 < z < 8 galaxies in the CANDELS GOODS-S, HUDF and HUDF parallel fields. Based on non-parametric measurements and incorporating a careful treatment of measurement biases, we quantify the typical size of galaxies at each redshift as the peak of the log-normal size distribution, rather than the arithmetic mean size. Parameterizing the evolution of galaxy half-light radius as $r_{50} \propto (1+z)^n$, we find $n = -0.20 \pm 0.26$ at bright UV-luminosities ($0.3L_{*(z=3)} < L < L_*$) and $n = -0.47 \pm 0.62$ at faint luminosities ($0.12L_* < L < 0.3L_*$). Furthermore, simulations based on artificially redshifting our z~4 galaxy sample show that we cannot reject the null hypothesis of no size evolution. We show that this result is caused by a combination of the size-dependent completeness of high-redshift galaxy samples and the underestimation of the sizes of the largest galaxies at a given epoch. To explore the evolution of galaxy morphology we first compare asymmetry measurements to those from a large sample of simulated single S\'ersic profiles, in order to robustly categorise galaxies as either `smooth' or `disturbed'. Comparing the disturbed fraction amongst bright ($M_{UV} \leq -20$) galaxies at each redshift to that obtained by artificially redshifting our z~4 galaxy sample, while carefully matching the size and UV-luminosity distributions, we find no clear evidence for evolution in galaxy morphology over the redshift interval 4 < z < 8. Therefore, based on our results, a bright ($M_{UV} \leq -20$) galaxy at z~6 is no more likely to be measured as `disturbed' than a comparable galaxy at z~4, given the current observational constraints.Comment: 29 pages, 25 figures, 4 tables, published in MNRA

Integrated J- and H-band spectra of globular clusters in the LMC: implications for stellar population models and galaxy age dating

(Abridged) The rest-frame near-IR spectra of intermediate age (1-2 Gyr) stellar populations are dominated by carbon based absorption features offering a wealth of information. Yet, spectral libraries that include the near-IR wavelength range do not sample a sufficiently broad range of ages and metallicities to allow for accurate calibration of stellar population models and thus the interpretation of the observations. In this paper we investigate the integrated J- and H-band spectra of six intermediate age (1-3 Gyr) and old (>10 Gyr) globular clusters in the Large Magellanic Cloud, using observations obtained with the SINFONI IFU at the VLT. H-band C2 and K-band 12CO(2-0) feature strengths are compared to the models of Maraston (2005). C2 is reasonably well reproduced by the models at all ages, while 12CO(2-0) shows good agreement for older (age>2 Gyr) populations, but the younger (1.3 Gyr) globular clusters do not follow the models. We argue that this is due to the fact that the empirical calibration of the models relies on only a few Milky Way carbon star spectra, which show different 12CO(2-0) index strengths than the LMC stars. The C2 absorption feature strength correlates strongly with age. It is present essentially only in populations that have 1-2 Gyr old stars, while its value is consistent with zero for older populations. The distinct spectral energy distribution observed for the intermediate age globular clusters in the J- and H-bands agrees well with the model predictions of Maraston for the contribution from the thermally pulsing asymptotic giant branch phase (TP-AGB). We show that the H-band C2 absorption feature and the J-, H-band spectral shape can be used as an age indicator for intermediate age stellar populations in integrated spectra of star clusters and galaxies.Comment: 10 pages, 6 figures, abstract abridged, accepted for publication in A&

Integrated K-band spectra of old and intermediate-age globular clusters in the Large Magellanic Cloud

Current stellar population models have arguably the largest uncertainties in the near-IR wavelength range, partly due to a lack of large and well calibrated empirical spectral libraries. In this paper we present a project, which aim it is to provide the first library of luminosity weighted integrated near-IR spectra of globular clusters to be used to test the current stellar population models and serve as calibrators for the future ones. Our pilot study presents spatially integrated K-band spectra of three old (>10 Gyr) and metal poor ([Fe/H]~-1.4), and three intermediate age (1-2 Gyr) and more metal rich ([Fe/H]~-0.4) globular clusters in the LMC. We measured the line strengths of the Na I, Ca I and 12CO(2-0) absorption features. The Na I index decreases with the increasing age and decreasing metallicity of the clusters. The Dco index, used to measure the 12CO(2-0) line strength, is significantly reduced by the presence of carbon-rich TP-AGB stars in the globular clusters with age ~1 Gyr. This is in contradiction with the predictions of the stellar population models of Maraston (2005). We find that this disagreement is due to the different CO absorption strength of carbon-rich Milky Way TP-AGB stars used in the models and the LMC carbon stars in our sample. For globular clusters with age >2 Gyr we find Dco index measurements consistent with the model predictions.Comment: 15 pages, 11 figures, accepted for publication in A&

Effectiveness of two video-based multicomponent treatments for fibromyalgia : The added value of cognitive restructuring and mindfulness in a three-arm randomised controlled trial

Acord transformatiu CRUE-CSICUTP en procés de revisióBackground/objectives: The aim of this study was to examine the effectiveness of two video-based multicomponent programs (FIBROWALK) and the Multicomponent Physiotherapy Program (MPP) for patients with fibromyalgia (FM) compared to treatment-as-usual (TAU) only. We posit that FIBROWALK, due to inclusion of specific psychological ingredients (cognitive restructuring and mindfulness), can produce additional clinical benefits when compared to TAU or MPP alone. Methods: A total of 330 patients with FM were recruited and randomly allocated (1:1:1) to TAU only, TAU + FIBROWALK, or TAU + MPP. FIBROWALK and MPP consisted of weekly videos on pain neuroscience education, therapeutic exercise and self-management patient education, but only the FIBROWALK intervention provided cognitive restructuring and mindfulness. Both programs were structurally equivalent. Between-group differences in functional impairment, pain, kinesiophobia, anxious-depressive symptoms and physical functioning were evaluated at post-treatment following Intention-To-Treat and complete-case approaches. Results: Compared to TAU only, individuals in the FIBROWALK arm showed larger improvements in all clinical outcomes; similarly, participants in the MPP program also showed greater improvements in functional impairment, perceived pain, kinesiophobia, depressive symptoms compared to TAU only. The FIBROWALK intervention showed superior effects in improving pain, anxiety and depressive symptoms and physical functioning compared to MPP. Conclusions: This RCT supports the short-term effectiveness of the video-based multicomponent programs FIBROWALK and MPP for FM and provides evidence that cognitive-behavioural and mindfulness-based techniques can be clinically useful in the context of physiotherapeutic multicomponent treatment programs. Trial registration number: NCT04571528

Ultra deep sub-kpc view of nearby massive compact galaxies

Using Gemini North telescope ultra deep and high resolution (sub-kpc) K-band adaptive optics imaging of a sample of 4 nearby (z~0.15) massive (~10^{11}M_sun) compact (R<1.5 kpc) galaxies, we have explored the structural properties of these rare objects with an unprecedented detail. Our surface brightness profiles expand over 12 magnitudes in range allowing us to explore the presence of any faint extended envelope on these objects down to stellar mass densities ~10^{6} M_sun/kpc^{2} at radial distances of ~15 kpc. We find no evidence for any extended faint tail altering the compactness of these galaxies. Our objects are elongated, resembling visually S0 galaxies, and have a central stellar mass density well above the stellar mass densities of objects with similar stellar mass but normal size in the present universe. If these massive compact objects will eventually transform into normal size galaxies, the processes driving this size growth will have to migrate around 2-3x10^{10}M_sun stellar mass from their inner (R<1.7 kpc) region towards their outskirts. Nearby massive compact galaxies share with high-z compact massive galaxies not only their stellar mass, size and velocity dispersion but also the shape of their profiles and the mean age of their stellar populations. This makes these singular galaxies unique laboratories to explore the early stages of the formation of massive galaxies.Comment: Accepted for publication in ApJ Letter. Version revised to match the accepted versio

Non-parametric analysis of the rest-frame UV sizes and morphological disturbance amongst L_* galaxies at 4 < z < 8

We present the results of a study investigating the sizes and morphologies of redshift 4 < z < 8 galaxies in the CANDELS (Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey) GOODS-S (Great Observatories Origins Deep Survey southern field), HUDF (Hubble Ultra-Deep Field) and HUDF parallel fields. Based on non-parametric measurements and incorporating a careful treatment of measurement biases, we quantify the typical size of galaxies at each redshift as the peak of the lognormal size distribution, rather than the arithmetic mean size. Parametrizing the evolution of galaxy half-light radius as r_(50) ∝ (1 + z)^n, we find n = −0.20 ± 0.26 at bright UV-luminosities (0.3L_*(z = 3) < L < L_*) and n = −0.47 ± 0.62 at faint luminosities (0.12L_* < L < 0.3L_*). Furthermore, simulations based on artificially redshifting our z ∼ 4 galaxy sample show that we cannot reject the null hypothesis of no size evolution. We show that this result is caused by a combination of the size-dependent completeness of high-redshift galaxy samples and the underestimation of the sizes of the largest galaxies at a given epoch. To explore the evolution of galaxy morphology we first compare asymmetry measurements to those from a large sample of simulated single Sérsic profiles, in order to robustly categorize galaxies as either ‘smooth’ or ‘disturbed’. Comparing the disturbed fraction amongst bright (M_(1500) ≤ −20) galaxies at each redshift to that obtained by artificially redshifting our z ∼ 4 galaxy sample, while carefully matching the size and UV-luminosity distributions, we find no clear evidence for evolution in galaxy morphology over the redshift interval 4 < z < 8. Therefore, based on our results, a bright (M_(1500) ≤ −20) galaxy at z ∼ 6 is no more likely to be measured as ‘disturbed’ than a comparable galaxy at z ∼ 4, given the current observational constraints