Escape Rooms as a Clinical Evaluation Method for Nursing Students

Background: There are currently no studies available about the possible use of gamification in the evaluation of nursing students’ clinical skills. The purpose of this study was to understand the gameful experience and satisfaction of nursing students in the evaluation of their clinical skills using an escape room. Methods: A quasiexperimental study was carried out. The participants were divided into an experimental group (escape room) and a control group. Results: The experimental group had higher than average scores in all dimensions of the gameful experience scale, except in the dimension of negative effects. Conclusions: Escape rooms are a useful tool for the evaluation of nursing students compared with using the objective structured clinical evaluation

Dust properties of Lyman break galaxies at z∼3z\sim3

We explore from a statistical point of view the far-infrared (far-IR) and sub-millimeter (sub-mm) properties of a large sample of LBGs (22,000) at z~3 in the COSMOS field. The large number of galaxies allows us to split it in several bins as a function of UV luminosity, UV slope, and stellar mass to better sample their variety. We perform stacking analysis in PACS (100 and 160 um), SPIRE (250, 350 and 500 um) and AzTEC (1.1 mm) images. Our stacking procedure corrects the biases induced by galaxy clustering and incompleteness of our input catalogue in dense regions. We obtain the full IR spectral energy distributions (SED) of subsamples of LBGs and derive the mean IR luminosity as a function of UV luminosity, UV slope, and stellar mass. The average IRX is roughly constant over the UV luminosity range, with a mean of 7.9 (1.8 mag). However, it is correlated with UV slope, and stellar mass. We investigate using a statistically-controlled stacking analysis as a function of (stellar mass, UV slope) the dispersion of the IRX-UVslope and IRX-M* plane. Our results enable us to study the average relation between star-formation rate (SFR) and stellar mass, and we show that our LBG sample lies on the main sequence of star formation at z~3.Comment: Accepted to A&A, 17 Pages, 14 Figures, 2 Table

Surgery on the wrong side: Implication for the patient and the professional. Experience in a Major Ambulatory Surgery of the Foot Unit

La cirugía del lado erróneo es una complicación poco frecuente en cirugía ortopédica, pero con serias consecuencias para el paciente, el cirujano y la institución sanitaria, debiéndose poner todas las medidas necesarias para evitar que se produzca. Hemos efectuado un estudio prospectivo de la implantación de un protocolo para prevenir la cirugía del lado erróneo en 101 pacientes intervenidos en la Unidad de Cirugía Mayor Ambulatoria (CMA) de cualquier patología del pie, realizándose tres marcajes independientes para la verificación del lado: por el paciente, la enfermera y el anestesista. Revisamos la existencia de la información del lado en los documentos de la historia vlínica (HC) y su correlación con el lado operado. Un 24,8% de los pacientes no fueron informados que tenían que realizarse una marca del pie a operar. Un 18,4% de los pacientes avisados no se marcaron, no existiendo relación con el sexo, edad, nivel de estudios, vivir solo o intervención previa de pies. En 37 pacientes existía una falta de anotación del lado en los documentos siendo más frecuente esta omisión en la HC de Cirugía Ortopédica y Traumatología y de Anestesiología. Se detectaron 9 casos de incongruencias de lado quirúrgico, todos en pacientes con cirugía previa de algún pie. El marcaje de lado se ha incorporado como una práctica rutinaria en la cirugía del pie, siendo beneficioso para la seguridad del paciente, debiéndose convertir en un futuro próximo en una conducta habitual en todas las áreas quirúrgicas

The alhambra survey: evolution of galaxy spectral segregation

We study the clustering of galaxies as a function of spectral type and redshift in the range 0.35 <z <1.1 using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data cover 2.381 deg2 in 7 fields, after applying a detailed angular selection mask, with accurate photometric redshifts down to IAB <24. From this catalog we draw five fixed number density redshift-limited bins. We estimate the clustering evolution for two different spectral populations selected using the ALHAMBRA-based photometric templates: quiescent and star-forming galaxies. For each sample we measure the real-space clustering using the projected correlation function. Our calculations are performed over the range [0.03, 10.0] h-1 Mpc, allowing us to find a steeper trend for Mpc, which is especially clear for star-forming galaxies. Our analysis also shows a clear early differentiation in the clustering properties of both populations: star-forming galaxies show weaker clustering with evolution in the correlation length over the analyzed redshift range, while quiescent galaxies show stronger clustering already at high redshifts and no appreciable evolution. We also perform the bias calculation where similar segregation is found, but now it is among the quiescent galaxies where a growing evolution with redshift is clearer (abrigatted). These findings clearly corroborate the well-known color-density relation, confirming that quiescent galaxies are mainly located in dark matter halos that are more massive than those typically populated by star-forming galaxies.Ministerio de Economía y Competitividad y FEDER AYA2010-22111-C03-02 AYA2013-48623-C2-2 AYA2012-39620 AYA2013-40611-P AYA2013-42227-P AYA2013-43188-P AYA2013-48623-C2-1 ESP2013-48274 AYA2014-58861-C3-1Junta de Andalucía TIC114 JA2828 P10-FQM-644

Logarithmic asymptotics of the densities of SPDEs driven by spatially correlated noise

We consider the family of stochastic partial differential equations indexed by a parameter \eps\in(0,1], \begin{equation*} Lu^{\eps}(t,x) = \eps\sigma(u^\eps(t,x))\dot{F}(t,x)+b(u^\eps(t,x)), \end{equation*} (t,x)\in(0,T]\times\Rd with suitable initial conditions. In this equation, $L$ is a second-order partial differential operator with constant coefficients, $\sigma$ and $b$ are smooth functions and $\dot{F}$ is a Gaussian noise, white in time and with a stationary correlation in space. Let p^\eps_{t,x} denote the density of the law of u^\eps(t,x) at a fixed point (t,x)\in(0,T]\times\Rd. We study the existence of \lim_{\eps\downarrow 0} \eps^2\log p^\eps_{t,x}(y) for a fixed $y\in\R$. The results apply to a class of stochastic wave equations with $d\in\{1,2,3\}$ and to a class of stochastic heat equations with $d\ge1$.Comment: 39 pages. Will be published in the book " Stochastic Analysis and Applications 2014. A volume in honour of Terry Lyons". Springer Verla

Stellar populations of galaxies in the ALHAMBRA survey up to z∼1z \sim 1. II. Stellar content of quiescent galaxies within the dust-corrected stellar mass−-colour and the UVJUVJ colour−-colour diagrams

Our aim is to determine the distribution of stellar population parameters (extinction, age, metallicity, and star formation rate) of quiescent galaxies within the rest-frame stellar mass$-$colour and $UVJ$ colour$-$colour diagrams corrected for extinction up to $z\sim1$. 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. We set constraints on the stellar population parameters of quiescent galaxies combining the ALHAMBRA multi-filter photo-spectra with our SED-fitting code MUFFIT, making use of composite stellar population 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 the LOESS method to reduce uncertainty effects. Quiescent galaxy samples defined via classical $UVJ$ diagrams are typically contaminated by a $\sim20$% fraction of DSF galaxies. A significant part of the galaxies in the green valley are actually obscured star-forming galaxies ($\sim30-65$%). 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.Comment: (37 pages, 29 figures, accepted for publication in A&A

VEHÍCULO AÉREO NO TRIPULADO EMPLEANDO HARDWARE RASPBERRY PI 3 PARA APLICACIÓN EN MONITOREO REMOTO (UNMANNED AERIAL VEHICLE USING RASPBERRY PI 3 HARDWARE FOR REMOTE MONITORING APPLICATION)

En los últimos años, el área de investigación de la Robótica Móvil ha sido el centro de atención de varias investigaciones, productos y prototipos debido a los beneficios prácticos que esta línea de investigación brinda a la vida cotidiana de los seres humanos. Nuevos productos y prototipos de la Robótica Móvil que generan asombro al mundo surgen todos los días, desde robots móviles con la habilidad para asistir a ubicar a una persona en un edificio derrumbado hasta robots que asisten a los astronautas en la estación espacial internacional (Dı́az Cantos, 2015). El objetivo de este trabajo es la elaboración de una herramienta que sea auxiliar en labores de monitoreo remoto en áreas cuya extensión sea mayor a las capacidades de desplazamiento humanas, o peligrosas para el mismo. En este trabajo se compone por las siguientes etapas: en la introducción, se describe brevemente la evolución y clasificación de los vehículos aéreos no tripulados mencionando la necesidad resuelta por este proyecto, las posibles aplicaciones de los VANT y metodología que se siguió con los nuevos componentes empleados en la implementación del VANT. En el apartado de los métodos y materiales se mencionan los pasos correspondientes en el diseño empleando el ordenador de placa reducida Raspberry Pi 3 model B como controladora de vuelo, de video e interfaz, junto con los sensores que realizan el monitoreo de las variables del entorno de operación del VANT. Tales variables son: temperatura, presión barométrica, humedad, orientación (basado en los ángulos de navegación roll, pitch y yaw), la posición relativa (mediante el uso de un acelerómetro) y una cámara para capturar el video. En la sección de los resultados y discusión se aborda el impacto causado por el trabajo; la razón del porque la tarjeta Raspberry Pi 3 model B no es recomendada para ser utilizada como controladora de vuelo, transmisión de video y alojamiento de la interfaz gráfica, ya que sus recursos son insuficientes para tener un adecuado control del VANT.Palabra(s) Clave: VANT, Control, Raspberry Pi, Monitoreo remoto, Interfaz. AbstractOn last years, the investigation area of the mobile robotics has been the center of attention for several investigations, products, and prototypes due to the practical benefits that this investigation line provides to the daily life and the human beings. New products and prototypes of the mobile robotics that awesome the world are created every day; from mobile robots with the ability to locate a person in a collapsed building to robots that assist astronauts in the International Space Station. This work's objective is the elaboration of an auxiliary tool in remote monitoring tasks in areas in which extension are superior to the human displacement capabilities or dangerous for the human being. This work is composed by the next stages: Introduction briefly describes the evolution and classification of the unmanned aerial vehicles doing mention in the necessity solved by this project; also the UAV possibles applications and the followed methodology with the new components used in the UAV implementation. In the Methods and materials section is mentioned the corresponding steps in the design using the reduced plate computer Raspberry Pi 3 model B as a flight controller, video controller, and user interface; which is implemented with a set of sensors that make a monitoring of the environment variables that intervene in the operation of the UAV such as temperature, barometric pressure, humidity, orientation (by the navigation angles roll, pitch, yaw), relative position (using an accelerometer) and a camera for capturing video. In the Results and Discussion sections, we approach to the impact caused by this work; the reason of why the computer Raspberry Pi 3 model B is not recommended for been used as a flight controller, video transmitter and graphic interface host, due to its resources are insufficient for having an adequate control for the UAV.Key word(s): VANT, Raspberry Pi, remote monitoring, interface, Control

The ALHAMBRA survey: evolution of galaxy spectral segregation

We study the clustering of galaxies as a function of spectral type and redshift in the range $0.35 < z < 1.1$ using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data cover 2.381 deg$^2$ in 7 fields, after applying a detailed angular selection mask, with accurate photometric redshifts [$\sigma_z < 0.014(1+z)$] down to $I_{AB} < 24$. From this catalog we draw five fixed number density, redshift-limited bins. We estimate the clustering evolution for two different spectral populations selected using the ALHAMBRA-based photometric templates: quiescent and star-forming galaxies. For each sample, we measure the real-space clustering using the projected correlation function. Our calculations are performed over the range $[0.03,10.0] h^{-1}$ Mpc, allowing us to find a steeper trend for $r_p \lesssim 0.2 h^{-1}$ Mpc, which is especially clear for star-forming galaxies. Our analysis also shows a clear early differentiation in the clustering properties of both populations: star-forming galaxies show weaker clustering with evolution in the correlation length over the analysed redshift range, while quiescent galaxies show stronger clustering already at high redshifts, and no appreciable evolution. We also perform the bias calculation where similar segregation is found, but now it is among the quiescent galaxies where a growing evolution with redshift is clearer. These findings clearly corroborate the well known colour-density relation, confirming that quiescent galaxies are mainly located in dark matter halos that are more massive than those typically populated by star-forming galaxies.Comment: 14 pages, 9 figures, accepted by Ap

The ALHAMBRA survey: Accurate merger fractions by PDF analysis of photometric close pairs

Our goal is to develop and test a novel methodology to compute accurate close pair fractions with photometric redshifts. We improve the current methodologies to estimate the merger fraction f_m from photometric redshifts by (i) using the full probability distribution functions (PDFs) of the sources in redshift space, (ii) including the variation in the luminosity of the sources with z in both the selection of the samples and in the luminosity ratio constrain, and (iii) splitting individual PDFs into red and blue spectral templates to deal robustly with colour selections. We test the performance of our new methodology with the PDFs provided by the ALHAMBRA photometric survey. The merger fractions and rates from the ALHAMBRA survey are in excellent agreement with those from spectroscopic work, both for the general population and for red and blue galaxies. With the merger rate of bright (M_B <= -20 - 1.1z) galaxies evolving as (1+z)^n, the power-law index n is larger for blue galaxies (n = 2.7 +- 0.5) than for red galaxies (n = 1.3 +- 0.4), confirming previous results. Integrating the merger rate over cosmic time, we find that the average number of mergers per galaxy since z = 1 is N_m = 0.57 +- 0.05 for red galaxies and N_m = 0.26 +- 0.02 for blue galaxies. Our new methodology exploits statistically all the available information provided by photometric redshift codes and provides accurate measurements of the merger fraction by close pairs only using photometric redshifts. Current and future photometric surveys will benefit of this new methodology.Comment: Submitted to A&A, 15 pages, 15 figures, 6 tables. Comments are welcome. Close pair systems available at https://cloud.iaa.csic.es/alhambra/catalogues/ClosePairs