La vivencia de la esclavitud: nota bibliográfica sobre testimonios y autobiografias de esclavos afroamericanos.

Sin resume

Clustering of galaxies: evolution, segregation and baryon acoustic oscillations

In this thesis, we tackle several open problems in the study of large-scale structure through the clustering of galaxies. To this end, we analyse data from some of the latest surveys, and we also develop new statistical techniques needed for this analysis in specific cases. In the first part, we focus on small and intermediate scales, where the relation between galaxy properties and their clustering (known as segregation) is important. The work in this part is driven by the exploitation of data from the ongoing Advanced Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) survey, which is perfectly suited to study the evolution of segregation trough cosmic time. We developed a method for the recovery of the real-space clustering from photometric surveys with the characteristics of ALHAMBRA. This method is based on the use of the projected correlation function, and is adapted to data with typical photometric redshift errors Dz < 0.015 (1+z). We tested the method using N-body simulations, and then applied it to the calculation of the correlation function for several samples drawn from the ALHAMBRA survey. We divided our sample in three redshift bins, and selected several galaxy samples in each of them based on B-band luminosity. In the range of scales studied, the correlation function for all samples was well fitted by a power law. We observed as well the effects of evolution, and of luminosity segregation. We also reviewed the basic tools available in the framework of the statistics of marked point processes to study galaxy segregation. We illustrated their application using a galaxy sample drawn from the 2dFGRS, characterised by a spectral classification parameter. We introduced the mark connection function, showing that it gives valuable information when analysing different galaxy populations defined by some set of galaxy characteristics. In the second part, we focus on the study of a large scale feature of the galaxy distribution, the baryon acoustic oscillations (BAO). We measured the two-point correlation function for several samples drawn from the largest surveys to date, 2dFGRS and SDSS. We obtained a peak corresponding to BAO at the expected scale in all cases, which shows the reliability of the detection of this feature. Finally, we developed a new method for the analysis of the BAO phenomenon. This method makes use of the possibilities of wavelets methods to look for the actual structures in configuration space which are responsible for the BAO. It is also based on the use of two complementary mass tracers, and we illustrated it using a catalogue formed by `Main' and Luminous Red Galaxy samples from SDSS. In this way, we showed how we were able not only to detect BAO in the samples, but also to localise regions giving lower or higher BAO signal. This kind of information is completely lost when using the traditional two-point statistics methods

Comentario: Una nota sobre la agricultura familiar y la naturaleza de las unidades productivas en agricultura

[ES] La tribuna de debate que Economía Agraria y Recursos Naturales dedica a la declaración por Naciones Unidas de 2014 como Año Internacional de la Agricultura Familiar (AIAF) me da ocasión para introducir en esta nota unos breves comentarios sobre este tema, tomando como base el artículo de Eduardo Moyano titulado “Agricultura familiar. Algunas reflexiones para un debate necesario” incluido en esta tribuna.Arnalte Alegre, E. (2014). Comentario: Una nota sobre la agricultura familiar y la naturaleza de las unidades productivas en agricultura. Economía Agraria y Recursos Naturales - Agricultural and Resource Economics. 14(1):141-146. https://doi.org/10.7201/earn.2014.01.08SWORD14114614

Joint constraints on galaxy bias and σ8\sigma_8 through the N-pdf of the galaxy number density

We present a full description of the N-probability density function of the galaxy number density fluctuations. This N-pdf is given in terms, on the one hand, of the cold dark matter correlations and, on the other hand, of the galaxy bias parameter. The method relies on the assumption commonly adopted that the dark matter density fluctuations follow a local non-linear transformation of the initial energy density perturbations. The N-pdf of the galaxy number density fluctuations allows for an optimal estimation of the bias parameter (e.g., via maximum-likelihood estimation, or Bayesian inference if there exists any a priori information on the bias parameter), and of those parameters defining the dark matter correlations, in particular its amplitude ($\sigma_8$). It also provides the proper framework to perform model selection between two competitive hypotheses. The parameters estimation capabilities of the N-pdf are proved by SDSS-like simulations (both ideal log-normal simulations and mocks obtained from Las Damas simulations), showing that our estimator is unbiased. We apply our formalism to the 7th release of the SDSS main sample (for a volume-limited subset with absolute magnitudes $M_r \leq -20$). We obtain $\hat{b} = 1.193 \pm 0.074$ and $\hat{\sigma_8} = 0.862 \pm 0.080$, for galaxy number density fluctuations in cells of a size of $30h^{-1}$Mpc. Different model selection criteria show that galaxy biasing is clearly favoured.Comment: 25 pages, 9 figures, 2 tables. v2: Substantial revision, adding the joint constraints with \sigma_8 and testing with Las Damas mocks. Matches version accepted for publication in JCA

Protocolo de tratamiento de la rinosinusitis crónica en adultos

Treball Final de Grau en Medicina. Codi: MD1158. Curs acadèmic: 2020/2021La rinosinusitis crónica (RSC) tiene una prevalencia del 11% en la población y supone un importante factor agravante para la salud de los afectados debido a su difícil control. Su limitado estudio etiológico y fisiopatológico hace que el correcto abordaje terapéutico todavía suponga hoy día, un reto. Sin embargo, la minuciosa caracterización de los pacientes puede ayudar a la elección óptima de los tratamientos, dando lugar a mejores resultados en el manejo de la patología. El actual Trabajo de Fin de Grado tiene como principal objetivo la elaboración de un protocolo terapéutico para la RSC dirigido a los servicios de Otorrinolaringología, Alergología y Farmacia del Hospital General Universitario de Castellón. Para llegar a ello se realizó una búsqueda bibliográfica con el fin de obtener la mejor evidencia disponible de los tratamientos actuales y posteriormente, generar las recomendaciones en base a las referencias estudiadas. Con ello se pretende determinar el correcto manejo de los pacientes para alcanzar así, mejoras en su calidad de vida.Chronic rhinosinusitis (CRS) has an 11% prevalence in society and entails an important aggravating health factor for the patients due to its difficult control. Its limited etiological and psychopathological study makes the correct therapeutic approach to its control still a challenge. Nevertheless, the thorough characterization of the patients can help the optimal choice of the treatments improving results in the pathology management. The present Degree Final Project has as major goal to elaborate a treatment protocol for CRS addressed to Otorhinolaryngology, Allergology and Pharmacy services of the General University Hospital of Castellón. To achieve this, a bibliographic research was carried out to get the best evidence available of the current treatments and later generate the recommendations based on the references obtained. This is intended to determine the management of this patients to achieve important improvements in their quality of life

Armonizador para instrumento musical

Este proyecto desarrolla una aplicación que permite generar una armonía a partir de una nota musical teniendo en cuenta la escala y la tonalidad. El trabajo está dividido en tres partes. Primero se desarrolla la aplicación con el programa MATLAB para simular todo el proceso utilizando archivos de audio, después se implementa con un procesador digital de señales de Texas Instruments para trabajar en tiempo real utilizando una guitarra eléctrica y finalmente se diseña una interfaz gráfica con el programa Visual C++ que permite al usuario interactuar con la aplicación desde un PC. Para trabajar en tiempo real se utiliza la técnica del doble buffer en la adquisición de datos de manera que se consigue reproducir la armonía a la vez que se toca el instrumento. Para generar una armonía se debe conocer en todo momento la frecuencia fundamental de la nota que se toca. En este trabajo se utiliza la técnica del enventanado y la transformada de Fourier para determinarla. Esto se hace con una ventana que recorre la señal al mismo tiempo que se calcula la transformada de Fourier. La elección del tamaño de la ventana junto con la frecuencia de muestreo juega un papel importante ya que determinan la resolución frecuencial, la resolución temporal y la frecuencia máxima que tiene la aplicación, o dicho de otra manera, determina el rango de notas del instrumento y la velocidad con que se pueden tocar. Con la transformada de Fourier se obtiene el espectro de frecuencias de la señal donde aplicando un algoritmo se consigue detectar la frecuencia fundamental. A partir de esta frecuencia se determinan las frecuencias del resto de notas que forman un acorde o un intervalo armónico. Además, conociendo la amplitud de la señal cada vez que se determina la frecuencia fundamental se puede caracterizar la envolvente de la nota. Después, usando una señal de 1 Hz se generan todas las señales que forman la armonía donde se suman para obtener la señal de salida. Entre los efectos que ofrece esta aplicación se encuentran los acordes de 10 escalas con 15 tonalidades por escala, intervalos de quinta, intervalos de quinta con octava, intervalos de octava, intervalos con dos octavas y la posibilidad de diseñar hasta tres intervalos armónicos simultáneos por nota a la elección del usuari

Shell-like structures in our cosmic neighbourhood

Signatures of the processes in the early Universe are imprinted in the cosmic web. Some of them may define shell-like structures characterised by typical scales. We search for shell-like structures in the distribution of nearby rich clusters of galaxies drawn from the SDSS DR8. We calculate the distance distributions between rich clusters of galaxies, and groups and clusters of various richness, look for the maxima in the distance distributions, and select candidates of shell-like structures. We analyse the space distribution of groups and clusters forming shell walls. We find six possible candidates of shell-like structures, in which galaxy clusters have maxima in the distance distribution to other galaxy groups and clusters at the distance of about 120 Mpc/h. The rich galaxy cluster A1795, the central cluster of the Bootes supercluster, has the highest maximum in the distance distribution of other groups and clusters around them at the distance of about 120 Mpc/h among our rich cluster sample, and another maximum at the distance of about 240 Mpc/h. The structures of galaxy systems causing the maxima at 120 Mpc/h form an almost complete shell of galaxy groups, clusters and superclusters. The richest systems in the nearby universe, the Sloan Great Wall, the Corona Borealis supercluster and the Ursa Major supercluster are among them. The probability that we obtain maxima like this from random distributions is lower than 0.001. Our results confirm that shell-like structures can be found in the distribution of nearby galaxies and their systems. The radii of the possible shells are larger than expected for a BAO shell (approximately 109 Mpc/h versus approximately 120 Mpc/h), and they are determined by very rich galaxy clusters and superclusters with high density contrast while BAO shells are barely seen in the galaxy distribution. We discuss possible consequences of these differences.Comment: Comments: 9 pages, 10 figures, Astronomy and Astrophysics, in pres

Clustering of galaxies: evolution, segregation, and baryon acoustic oscillations

In this thesis, we tackle several open problems in the study of large-scale structure through the clustering of galaxies. To this end, we analyse data from some of the latest surveys, and we also develop new statistical techniques needed for this analysis in specific cases. In the first part, we focus on small and intermediate scales, where the relation between galaxy properties and their clustering (known as segregation) is important. The work in this part is driven by the exploitation of data from the ongoing Advanced Large Homogeneous Area Medium-Band Redshift Astronomical (ALHAMBRA) survey, which is perfectly suited to study the evolution of segregation trough cosmic time. We developed a method for the recovery of the real-space clustering from photometric surveys with the characteristics of ALHAMBRA. This method is based on the use of the projected correlation function, and is adapted to data with typical photometric redshift errors Dz < 0.015 (1+z). We tested the method using N-body simulations, and then applied it to the calculation of the correlation function for several samples drawn from the ALHAMBRA survey. We divided our sample in three redshift bins, and selected several galaxy samples in each of them based on B-band luminosity. In the range of scales studied, the correlation function for all samples was well fitted by a power law. We observed as well the effects of evolution, and of luminosity segregation. We also reviewed the basic tools available in the framework of the statistics of marked point processes to study galaxy segregation. We illustrated their application using a galaxy sample drawn from the 2dFGRS, characterised by a spectral classification parameter. We introduced the mark connection function, showing that it gives valuable information when analysing different galaxy populations defined by some set of galaxy characteristics. In the second part, we focus on the study of a large scale feature of the galaxy distribution, the baryon acoustic oscillations (BAO). We measured the two-point correlation function for several samples drawn from the largest surveys to date, 2dFGRS and SDSS. We obtained a peak corresponding to BAO at the expected scale in all cases, which shows the reliability of the detection of this feature. Finally, we developed a new method for the analysis of the BAO phenomenon. This method makes use of the possibilities of wavelets methods to look for the actual structures in configuration space which are responsible for the BAO. It is also based on the use of two complementary mass tracers, and we illustrated it using a catalogue formed by `Main' and Luminous Red Galaxy samples from SDSS. In this way, we showed how we were able not only to detect BAO in the samples, but also to localise regions giving lower or higher BAO signal. This kind of information is completely lost when using the traditional two-point statistics methods.Peer Reviewe