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INTRODUCCIÓN: la mayoría de las investigaciones del crecimiento facial se enfocan hacia la documentación y predicción del crecimiento puberal opacando la descripción del crecimiento antes de los 12 años de edad. Aunque hay varias investigaciones en poblaciones caucásicas que han reportado los picos tempranos de crecimiento, ninguna lo ha ubicado y dimensionado con relación al pico puberal. En mestizos latinoamericanos no hay estudios reportados en la literatura. MÉTODOS: desde 1992 el Grupo de Investigación de Labio y Paladar Hendido, Fisiología Oral y Crecimiento Craneofacial, CES-LPH, está haciendo un estudio longitudinal del crecimiento facial en 44 mestizos colombianos sin tratamiento con una muestra de 373 radiografías cefálicas laterales obtenidas durante 18 años de seguimiento. RESULTADOS: de las 28 niñas de la muestra, 21 (75%) presentaron incrementos bienal mayores de 5 mm en la altura facial anterior (AFA) antes de los 12 años. En la altura facial posterior (AFP) hubo 9 (32%) niñas con incrementos bienales mayores a 5 mm antes de los 9 años. En 7 (43%) niños se presentaron incrementos bienales mayores a 5 mm en AFA antes de los 12 años y para la AFP hubo 9 (56%) niños con el mismo comportamiento antes de los 12 años. Para 5 de las niñas y 3 de los niños (18%), este fue el mayor pico de crecimiento en todo el seguimiento de la muestra desde los 6 hasta los 19 años, hallazgo no reportado anteriormente en la literatura. CONCLUSIONES: los picos tempranos de crecimiento vertical (AFA y AFP) en niños menores de 9 años pueden explicar el éxito de las terapias tempranas de ortopedia funcional de los maxilares.

Se expone el caso de una perra Bulldog Inglés que presentaba una gestación aproximada de 36 a 38 días, con secreción sanguinopurulenta por vulva y decaimiento, siendo éstos los únicos hallazgos al examen físico general. Al realizar procedimientos diagnósticos complementarios se evidenció que había productos vivos en un cuerno uterino y el otro estaba ocupado por fluido.Simultaneous pyometra and gestation in a bitch

The diagnostic tools in Dentistry that includes sequential measurements present several problems concerning its reliability, due to the techniques and human factors. Among those variables, there are some static such as cephalometric, anthropometric or dental studies and some functional such as those that evaluate electrical and mechanical activity of the craniofacial muscles. Objective: the aim of the study was to evaluate the reliability of the measurement criteria of the Upper Orbicularis Oris muscle electromyographic activity registration (AEMG) during swallowing and phonation in two sessions separated by 8 days. Materials and Methods: 15 healthy subjects of both sex between 18 and 25 year old participated in the study. The swallowing and phonation were evaluated with superficial electromyography (EMG), three times a session with a resting time of 60 seconds between them in two different days separated by 8 days. Results: the obtained data presented in the study show a high reliability of the Upper Orbicularis Oris muscle during phonation and swallowing for the numerical integration and for the normalized RMS in the time as well.

Este articulo presenta una revision de la computacion evolutiva como una alternativa en la generaciOn de conocimiento, se exploran los conceptos basicos de la tecnica y algunas aplicaciones en ciencias de la salud. Se presentan los mas importantes aspectos en la modelacion de sistemas y procesos biolagicos. Estos modelos pueden ser utilizados para la toma de decisiones en la vida real.

Background: Venous thromboembolism is a common disease seen in the emergency department and a cause of high morbidity and mortality, constituting a major health problem. Objectives: To assess the potential benefit of follow-up ultrasound of patients who attended the emergency department with suspected superficial venous thrombosis or deep venous thrombosis and were found to have an initial negative whole-leg (or arm) ultrasound study. Methods: This retrospective study included patients aged 18 years or older who were consecutively referred to a thrombosis clinic from the emergency department, with abnormal D-dimer test and moderate to high pre-test probability of deep venous thrombosis (Well's score ≥ 1), but a negative whole-leg (or arm) ultrasound. Demographic characteristics, symptom duration, laboratory and ultrasound data were recorded. At one-week follow-up, an experienced physician repeated ultrasound, and recorded the findings. Results: From January 2017 to April 2018, 54 patients were evaluated. The mean age was 66.8 years (SD 15.0) and 63% were women. The average D-dimer was 2159.9 (SD 3772.0) ng/mL. Ultrasound abnormalities were found in 12 patients (22.2%; 95% confidence interval of 12.5 to 36.0%), with 4 patients having proximal deep venous thrombosis, distal deep venous thrombosis in 2 patients and superficial venous thrombosis in 6 patients. We did not find any significant differences in demographic characteristics, venous thromboembolism risk factors or laboratory parameters between patients with negative and positive follow-up ultrasound. Conclusions: These preliminary findings suggest that a negative whole-leg (or arm) ultrasound in addition to an abnormal D-dimer in moderate to high deep venous thrombosis pretest probability patients, might be an insufficient diagnostic approach to exclude suspected deep venous thrombosis or superficial venous thrombosis. Confirmation of this higher than expected prevalence would support the need to repeat one-week ultrasound control in this population. [ABSTRACT FROM AUTHOR]

Aims. Our aim is to determine the distribution of stellar population parameters (extinction, age, metallicity, and star formation rates) of quiescent galaxies within the rest-frame stellar mass–colour diagrams and UVJ colour–colour diagrams corrected for extinction up to z ∼ 1. These novel diagrams reduce the contamination in samples of quiescent galaxies owing to dust-reddened galaxies, and they provide useful constraints on stellar population parameters only using rest-frame colours and/or stellar mass. Methods. We set constraints on the stellar population parameters of quiescent galaxies combining the ALHAMBRA multi-filter photo-spectra with our fitting code for spectral energy distribution, MUlti-Filter FITting (MUFFIT), making use of composite stellar population models based on two independent sets of simple stellar population (SSP) models. The extinction obtained by MUFFIT allowed us to remove dusty star-forming (DSF) galaxies from the sample of red UVJ galaxies. The distributions of stellar population parameters across these rest-frame diagrams are revealed after the dust correction and are fitted by LOESS, a bi-dimensional and locally weighted regression method, to reduce uncertainty effects. Results. Quiescent galaxy samples defined via classical UVJ diagrams are typically contaminated by a ∼20% fraction of DSF galaxies. A significant part of the galaxies in the green valley are actually obscured star-forming galaxies (∼30–65%). Consequently, the transition of galaxies from the blue cloud to the red sequence, and hence the related mechanisms for quenching, seems to be much more efficient and faster than previously reported. The rest-frame stellar mass–colour and UVJ colour–colour diagrams are useful for constraining the age, metallicity, extinction, and star formation rate of quiescent galaxies by only their redshift, rest-frame colours, and/or stellar mass. Dust correction plays an important role in understanding how quiescent galaxies are distributed in these diagrams and is key to performing a pure selection of quiescent galaxies via intrinsic colours. [ABSTRACT FROM AUTHOR]

Aims. We aim at constraining the stellar population properties of quiescent galaxies. These properties reveal how these galaxies evolved and assembled since z ∼ 1 up to the present time. Methods. Combining the ALHAMBRA multi-filter photo-spectra with the fitting code for spectral energy distribution MUFFIT (MUlti-Filter FITting), we built a complete catalogue of quiescent galaxies via the dust-corrected stellar mass vs. colour diagram. This catalogue includes stellar population properties, such as age, metallicity, extinction, stellar mass, and photometric redshift, retrieved from the analysis of composited populations based on two independent sets of simple stellar population (SSP) models. We developed and applied a novel methodology to provide, for the first time, the analytic probability distribution functions (PDFs) of mass-weighted age, metallicity, and extinction of quiescent galaxies as a function of redshift and stellar mass. We adopted different star formation histories to discard potential systematics in the analysis. Results. The number density of quiescent galaxies is found to increase since z ∼ 1, with a more substantial variation at lower stellar mass. Quiescent galaxies feature extinction AV <  0.6, with median values in the range AV = 0.15–0.3. At increasing stellar mass, quiescent galaxies are older and more metal rich since z ∼ 1. A detailed analysis of the PDFs reveals that the evolution of quiescent galaxies is not compatible with passive evolution and a slight decrease of 0.1–0.2 dex is hinted at median metallicity. The intrinsic dispersion of the age and metallicity PDFs show a dependence on stellar mass and/or redshift. These results are consistent with both sets of SSP models and assumptions of alternative star formation histories explored. Consequently, the quiescent population must undergo an evolutive pathway including mergers and/or remnants of star formation to reconcile the observed trends, where the "progenitor" bias should also be taken into account. [ABSTRACT FROM AUTHOR]

Context. Knowing the exact shape of the ultraviolet (UV) luminosity function (LF) of high-redshift galaxies is important to understand the star formation history of the early Universe. However, the uncertainties, especially at the faint and bright ends of the LFs, remain significant. Aims. In this paper, we study the UV LF of redshift z = 2.5 – 4.5 galaxies in 2.38 deg2 of ALHAMBRA data with I ≤ 24. Thanks to the large area covered by ALHAMBRA, we particularly constrain the bright end of the LF. We also calculate the cosmic variance and the corresponding bias values for our sample and derive their host dark matter halo masses. Methods. We have used a novel methodology based on redshift and magnitude probability distribution functions (PDFs). This methodology robustly takes into account the uncertainties due to redshift and magnitude errors, shot noise, and cosmic variance, and models the LF in two dimensions (z, MUV). Results. We find an excess of bright * M*UV ~ M UV * $\tilde{\ }M_{\rm{UV}}^{*}$ galaxies as compared to the studies based on broad-band photometric data. However, our results agree well with the LF of the magnitude-selected spectroscopic VVDS data. We measure high bias values, b ~ 8 – 10, that are compatible with the previous measurements considering the redshifts and magnitudes of our galaxies and further reinforce the real high-redshift nature of our bright galaxies. Conclusions. We call into question the shape of the LF at its bright end; is it a double power-law as suggested by the recent broad-band photometric studies or rather a brighter Schechter function, as suggested by our multi-filter analysis and the spectroscopic VVDS data. [ABSTRACT FROM AUTHOR]

The original ALHAMBRA catalogue contained over 400 000 galaxies selected using a synthetic F814W image, to the magnitude limit AB(F814W) ≈ 24.5. Given the photometric redshift depth of the ALHAMBRA multiband data ( = 0.86) and the approximately I-band selection, there is a noticeable bias against red objects at moderate redshift. We avoid this bias by creating a new catalogue selected in the Ks band. This newly obtained catalogue is certainly shallower in terms of apparent magnitude, but deeper in terms of redshift, with a significant population of red objects at z > 1. We select objects using the Ks band images, which reach an approximate AB magnitude limit Ks ≈ 22. We generate masks and derive completeness functions to characterize the sample. We have tested the quality of the photometry and photometric redshifts using both internal and external checks. Our final catalogue includes ≈95 000 sources down to Ks ≈ 22, with a significant tail towards high redshift. We have checked that there is a large sample of objects with spectral energy distributions that correspond to that of massive, passively evolving galaxies at z > 1, reaching as far as z ≈ 2.5. We have tested the possibility of combining our data with deep infrared observations at longer wavelengths, particularly Spitzer IRAC data. [ABSTRACT FROM AUTHOR]

Background and Aims The safety of foods and beverages is a prerequisite for consumers. The aim of this study is to check whether a low concentration of pesticide residues can be further reduced with the addition of a low dose of charcoal during white fermentation. Methods and Results Thirteen fungicides, boscalid, cyprodinil, fludioxonil, fenhexamide, pyrimethanil, cyazofamid, dimethomorph, fluopicolide, iprovalicarb, metrafenone, penconazole, spiroxamine and trifloxystrobin, were added together to five well-clarified and stabilised juices to reach a final fungicide concentration in juice slightly higher than that observed in bottled wines. Juices were fermented with two types of charcoal, both added at 20 and 50 mg/L. The course of fermentation was monitored, and the concentration of residual fungicides and of fermentative aromas was analysed by ultra-high performance liquid chromatography-MS/MS and GC-flame ionisation detector, respectively. Conclusions Charcoal removed up to 130 µg/L of fungicides. Compared with the control wines, those fermented with charcoal had 30-80% less fungicides. Only iprovalicarb was not significantly reduced. Aroma composition was not affected. Significance of the Study Low doses of charcoal added during fermentation can positively contribute to wine safety without penalising aroma and colour. [ABSTRACT FROM AUTHOR]

We consistently analyse for the first time the impact of survey depth and spatial resolution on the most used morphological parameters for classifying galaxies through non-parametric methods: Abraham and Conselice-Bershady concentration indices, Gini,M20moment of light, asymmetry, and smoothness. Three different non-local data sets are used, Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) and Subaru/XMMNewton Deep Survey (SXDS, examples of deep ground-based surveys), and Cosmos Evolution Survey (COSMOS, deep space-based survey). We used a sample of 3000 local, visually classified galaxies, measuring their morphological parameters at their real redshifts (z ~0). Then we simulated them to match the redshift and magnitude distributions of galaxies in the non-local surveys. The comparisons of the two sets allow us to put constraints on the use of each parameter for morphological classification and evaluate the effectiveness of the commonly used morphological diagnostic diagrams. All analysed parameters suffer from biases related to spatial resolution and depth, the impact of the former being much stronger. When including asymmetry and smoothness in classification diagrams, the noise effects must be taken into account carefully, especially for ground-based surveys. M20 is significantly affected, changing both the shape and range of its distribution at all brightness levels. We suggest that diagnostic diagrams based on 2-3 parameters should be avoided when classifying galaxies in ground-based surveys, independently of their brightness; for COSMOS they should be avoided for galaxies fainter than F814 = 23.0. These results can be applied directly to surveys similar to ALHAMBRA, SXDS and COSMOS, and also can serve as an upper/lower limit for shallower/deeper ones. [ABSTRACT FROM AUTHOR]