The Climate-system Historical Forecast Project: do stratosphere-resolving models make better seasonal climate predictions in boreal winter?

Using an international, multi-model suite of historical forecasts from the World Climate Research Programme (WCRP) Climate-system Historical Forecast Project (CHFP), we compare the seasonal prediction skill in boreal wintertime between models that resolve the stratosphere and its dynamics (high-top') and models that do not (low-top'). We evaluate hindcasts that are initialized in November, and examine the model biases in the stratosphere and how they relate to boreal wintertime (December-March) seasonal forecast skill. We are unable to detect more skill in the high-top ensemble-mean than the low-top ensemble-mean in forecasting the wintertime North Atlantic Oscillation, but model performance varies widely. Increasing the ensemble size clearly increases the skill for a given model. We then examine two major processes involving stratosphere-troposphere interactions (the El Niño/Southern Oscillation (ENSO) and the Quasi-Biennial Oscillation (QBO)) and how they relate to predictive skill on intraseasonal to seasonal time-scales, particularly over the North Atlantic and Eurasia regions. High-top models tend to have a more realistic stratospheric response to El Niño and the QBO compared to low-top models. Enhanced conditional wintertime skill over high latitudes and the North Atlantic region during winters with El Niño conditions suggests a possible role for a stratospheric pathway.

Characterizing the satellites of massive galaxies up to z ∼ 2: young populations to build the outskirts of nearby massive galaxies

The accretion of minor satellites is currently proposed as the most likely mechanism to explain the significant size evolution of the massive galaxies during the last ∼10 Gyr. In this paper, we investigate the rest-frame colours and the average stellar ages of satellites found around massive galaxies (M_star ∼ 10^11 M_⊙) since z ∼ 2. We find that the satellites have bluer colours than their central galaxies. When exploring the stellar ages of the galaxies, we find that the satellites have similar ages to the massive galaxies that host them at high redshifts, while at lower redshifts they are, on average, ≳1.5 Gyr younger. If our satellite galaxies create the envelope of nearby massive galaxies, our results would be compatible with the idea that the outskirts of those galaxies are slightly younger, metal-poorer and with lower [α/Fe] abundance ratios than their inner regions.

Testing diagnostics of nuclear activity and star formation in galaxies at z > 1

We present some of the first science data with the new Keck/MOSFIRE instrument to test the effectiveness of different AGN/SF diagnostics at z ~ 1.5. MOSFIRE spectra were obtained in three H-band multi-slit masks in the GOODS-S field, resulting in 2 hr exposures of 36 emission-line galaxies. We compare X-ray data with the traditional emission-line ratio diagnostics and the alternative mass-excitation and color-excitation diagrams, combining new MOSFIRE infrared data with previous HST/WFC3 infrared spectra (from the 3D-HST survey) and multiwavelength photometry. We demonstrate that a high [O III]/Hβ ratio is insufficient as an active galactic nucleus (AGN) indicator at z > 1. For the four X-ray-detected galaxies, the classic diagnostics ([O III]/Hβ versus [N II]/Hα and [S II]/Hα) remain consistent with X-ray AGN/SF classification. The X-ray data also suggest that "composite" galaxies (with intermediate AGN/SF classification) host bona fide AGNs. Nearly ~2/3 of the z ~ 1.5 emission-line galaxies have nuclear activity detected by either X-rays or the classic diagnostics. Compared to the X-ray and line ratio classifications, the mass-excitation method remains effective at z > 1, but we show that the color-excitation method requires a new calibration to successfully identify AGNs at these redshifts.

The evolutionary paths among galaxy types on the red sequence at 0.3 < Z < 1.5

We have studied the main evolutionary paths among the galaxy types residing on the massive end of the Red Sequence and nearby locations on the Green Valley during the last ∼9 Gyr. The morphological and star formation properties of a sample of these galaxies at 0 . 3 < z < 1 .5 with stellar masses M_∗ > 5 × 10^10 M_⊙ have been analysed. We present direct observational evidence for the first time of the existence of two main evolutionary paths among the different red galaxy types since z ∼ 1 .5, which provide some clues on the nature of the processes that have governed the assembly of present-day massive quiescent galaxies. The results are in excellent agreement with the hierarchical evolutionary framework proposed in the Eliche-Moral et al. (2010) model. Data from SHARDS (one of the ESO/GTC Large Programmes approved in 2009A) will complement and improve the present findings, shedding some light into many of the still unsettled questions concerning the migration of galaxies from the Blue Cloud to the Red Sequence at z < 1 .5.

Caracterización de la emisión de muy alta energía de los púlsares con los telescopios Magic

En 1967, la estudiante de doctorado Jocelyn Bell Burnell, observ o por primera vez la se~nal procedente de un p ulsar. Estos objetos estelares han sido desde entonces intensamente estudiados a todas las longitudes de onda. Debido a su intenso campo magn etico y gravitatorio, los p ulsares se han convertido en uno de los mejores laboratorios para el estudio de la materia en condiciones extremas. Recientemente, la detecci on de emisi on de muy alta energ as (VHE > 100 GeV) del p ulsar del Cangrejo ha obligado a replantearnos nuestras ideas sobre el funcionamiento de estas estrellas, ya que tal emisi on parec a descartada a priori por los modelos te oricos existentes. Estos modelos proponen distintos lugares en las magnetosferas de los p ulsares, y en torno a estas, como origen de la emisi on de muy alta energ a detectada, cada uno con caracter sticas propias en la distribuci on espectrales de energ a y en las curva de luz esperadas. Las observaciones de los p ulsares a muy altas energ as son por lo tanto fundamentales para entender la ubicaci on y los mecanismos de la emisi on y distinguir entre los distintos modelos. Esta tesis trata de la caracterizaci on de la emisi on de muy alta energ a de los p ulsares. Este estudio est a basado en las observaciones de p ulsares con los telescopios MAGIC y Fermi-LAT y en una estimaci on anal tica de la e ciencia de emisi on en rayos X y rayos gamma de los p ulsares en el contexto del modelo del \outer gap" o de \zona externa"...

Red de coordinación y seguimiento del primer curso del Grado en Ing. Sonido e Imagen en Telecomunicación (GISIT) de la Escuela Politécnica Superior

El profesorado de la red docente durante el curso 2011/12 ha realizado un proyecto coordinar las las asignaturas del primer curso del Grado en Ingeniería en Sonido e Imagen en Telecomunicación de la Escuela Politécnica Superior. Se ha realizado una puesta en común con los coordinadores de todos los cursos para realizar las recomendaciones de matriculación a los estudiantes que realizan su matricula a tiempo parcial o no superan cada curso todos los créditos matriculados. Se ha realizado un ajuste de los temarios con las asignaturas que comienzan su implantación en el siguiente curso y por otro lado una coordinación en la evaluación para eliminar las numerosas coincidencias de evaluaciones continuas, de diferentes actividades en cada semana.

Coordinación y seguimiento de los tres primeros cursos del Grado en Ing. Sonido e Imagen en Telecomunicación

El reto de implantar los nuevos grados exige un continuado esfuerzo de coordinación de las asignaturas de cada curso y de los diferentes cursos entres sí. En este trabajo se presentan los resultados de los diferentes proyectos que se han realizado para coordinar las asignaturas de los tres primeros cursos del Grado en Ingeniería en Sonido e Imagen en Telecomunicación de la Escuela Politécnica Superior. Además se analiza la coordinación de los proyectos entre sí, analizando los cambios surgidos en las fichas de las asignaturas, evaluación, metodología, etc. También se presenta una puesta en común con los coordinadores de todos los cursos para realizar las recomendaciones de matriculación a los estudiantes que realizan su matrícula a tiempo parcial o no superan cada curso todos los créditos matriculados. Y por último, se estudia la continuidad con los contenidos de las asignaturas que comienzan su implantación en el siguiente curso y por otro lado la coordinación en la evaluación para eliminar las numerosas coincidencias de evaluaciones continuas, de diferentes actividades en cada semana.

Seguimiento de las materias de Física en las titulaciones de Grado y Máster orientados a las tecnologías

El presente trabajo es resultado de un proyecto correspondiente a ediciones anteriores del programa Redes, que permitió la creación de un repositorio virtual que albergue el material elaborado por los profesores de las asignaturas de Física en las titulaciones de Grado. Actualmente, y debido a la motivación de los participantes, se está trabajando en poner al día el material correspondiente a los Grados y ampliarlo a las asignaturas Máster orientados a las tecnologías que se imparten en la Escuela Politécnica Superior de la Universidad de Alicante. El material recopilado es accesible virtualmente por todo el profesorado del departamento implicado en las asignaturas de Física, por medio de un repositorio virtual. Por otro lado, terminada una primera parte del trabajo nos encontramos inmersos en una reflexión sobre las metodologías aplicadas a partir del diálogo y la discusión entre los docentes sobre la experiencia en el aula con los alumnos y con los materiales generados.

Estudio de las capacidades de los estudiantes de nuevo ingreso en la asignatura de Física en las titulaciones de ingeniería

La red de investigación docente que se ha desarrollado en el curso 2007/08 se puede enmarcar dentro del ámbito de los créditos ECTS. Tiene como base la implementación de metodologías de trabajo durante dos semanas, no con conocimientos nuevos, sino con competencias adquiridas y necesarias para comprender los objetivos de la titulación, específicamente impartidos en las asignaturas de Física. La idea es obtener una valoración de la necesidad y consecuencia de los cursos de inicio puestos en marcha por la Universidad de Alicante y mantenidos por la Escuela Politécnica Superior. De esta forma mediante la realización y análisis de encuestas hemos analizado tanto la percepción de los alumnos respecto a estos cursos como la utilidad de los mismos. Para ello se han elaborado más de 600 encuestas y se ha contado con la participación de unos 500 alumnos. Además hemos estudiado que diferencias existen entre los resultados de los alumnos que han participado en el curso propuesto por la Escuela Politécnica y los demás. Por último hemos analizado como han mejorado los resultados de los alumnos antes y después del curso de inicio.

An accurate distance scale to the extremely massive cluster Stephenson 2

Discoveries during the last two years have revealed the existence of a vast region of star formation close to the base of the Scutum Arm, where at least five clusters of red supergiants have been found. In order to understand the nature of this region, we need to determine accurate distances to the clusters. We present here the first results of an ongoing program to derive fundamental parameters (such as age, distance, etc.) to the massive cluster Stephenson 2 studying for the first time its main sequence stars.

Infrared identification of 2XMM J191043.4+091629.4

Context. We report the infrared identification of the X-ray source 2XMM J191043.4+091629.4, which was detected by XMM-Newton/EPIC in the vicinity of the Galactic supernova remnant W49B. Aims. The aim of this work is to establish the nature of the X-ray source 2XMM J191043.4+091629.4 studying both the infrared photometry and spectroscopy of the companion. Methods. We analysed UKIDSS images around the best position of the X-ray source and obtained spectra of the best candidate using NICS in the Telescopio Nazionale Galileo (TNG) 3.5-m telescope. We present photometric and spectroscopic TNG analyses of the infrared counterpart of the X-ray source, identifying emission lines in the K-band. The H-band spectra does not present any significant feature. Results. We have shown that the Brackett γ H i at 2.165 μm, and He i at 2.184 μm and at 2.058 μm are significantly present in the infrared spectrum. The CO bands are also absent from our spectrum. Based on these results and the X-ray characteristics of the source, we conclude that the infrared counterpart is an early B-type supergiant star with an E(B − V) = 7.6 ± 0.3 at a distance of 16.0 ± 0.5 kpc. This would be, therefore, the first high-mass X-ray binary in the Outer Arm at galactic longitudes of between 30° and 60°.

Force-free twisted magnetospheres of neutron stars

Context. The X-ray spectra observed in the persistent emission of magnetars are evidence for the existence of a magnetosphere. The high-energy part of the spectra is explained by resonant cyclotron upscattering of soft thermal photons in a twisted magnetosphere, which has motivated an increasing number of efforts to improve and generalize existing magnetosphere models. Aims. We want to build more general configurations of twisted, force-free magnetospheres as a first step to understanding the role played by the magnetic field geometry in the observed spectra. Methods. First we reviewed and extended previous analytical works to assess the viability and limitations of semi-analytical approaches. Second, we built a numerical code able to relax an initial configuration of a nonrotating magnetosphere to a force-free geometry, provided any arbitrary form of the magnetic field at the star surface. The numerical code is based on a finite-difference time-domain, divergence-free, and conservative scheme, based of the magneto-frictional method used in other scenarios. Results. We obtain new numerical configurations of twisted magnetospheres, with distributions of twist and currents that differ from previous analytical solutions. The range of global twist of the new family of solutions is similar to the existing semi-analytical models (up to some radians), but the achieved geometry may be quite different. Conclusions. The geometry of twisted, force-free magnetospheres shows a wider variety of possibilities than previously considered. This has implications for the observed spectra and opens the possibility of implementing alternative models in simulations of radiative transfer aiming at providing spectra to be compared with observations.

Pulsar timing irregularities and the imprint of magnetic field evolution

Context. The rotational evolution of isolated neutron stars is dominated by the magnetic field anchored to the solid crust of the star. Assuming that the core field evolves on much longer timescales, the crustal field evolves mainly though Ohmic dissipation and the Hall drift, and it may be subject to relatively rapid changes with remarkable effects on the observed timing properties. Aims. We investigate whether changes of the magnetic field structure and strength during the star evolution may have observable consequences in the braking index n. This is the most sensitive quantity to reflect small variations of the timing properties that are caused by magnetic field rearrangements. Methods. We performed axisymmetric, long-term simulations of the magneto-thermal evolution of neutron stars with state-of-the-art microphysical inputs to calculate the evolution of the braking index. Relatively rapid magnetic field modifications can be expected only in the crust of neutron stars, where we focus our study. Results. We find that the effect of the magnetic field evolution on the braking index can be divided into three qualitatively different stages depending on the age and the internal temperature: a first stage that may be different for standard pulsars (with n ~ 3) or low field neutron stars that accreted fallback matter during the supernova explosion (systematically n < 3); in a second stage, the evolution is governed by almost pure Ohmic field decay, and a braking index n > 3 is expected; in the third stage, at late times, when the interior temperature has dropped to very low values, Hall oscillatory modes in the neutron star crust result in braking indices of a high absolute value and both positive and negative signs. Conclusions. Current magneto-thermal evolution models predict a large contribution to the timing noise and, in particular, to the braking index, from temporal variations of the magnetic field. Models with strong (≳ 1014 G) multipolar or toroidal components, even with a weak (~1012 G) dipolar field are consistent with the observed trend of the timing properties.

A new code for the Hall-driven magnetic evolution of neutron stars

Over the past decade, the numerical modeling of the magnetic field evolution in astrophysical scenarios has become an increasingly important field. In the crystallized crust of neutron stars the evolution of the magnetic field is governed by the Hall induction equation. In this equation the relative contribution of the two terms (Hall term and Ohmic dissipation) varies depending on the local conditions of temperature and magnetic field strength. This results in the transition from the purely parabolic character of the equations to the hyperbolic regime as the magnetic Reynolds number increases, which presents severe numerical problems. Up to now, most attempts to study this problem were based on spectral methods, but they failed in representing the transition to large magnetic Reynolds numbers. We present a new code based on upwind finite differences techniques that can handle situations with arbitrary low magnetic diffusivity and it is suitable for studying the formation of sharp current sheets during the evolution. The code is thoroughly tested in different limits and used to illustrate the evolution of the crustal magnetic field in a neutron star in some representative cases. Our code, coupled to cooling codes, can be used to perform long-term simulations of the magneto-thermal evolution of neutron stars.