La arqueología de la Edad del Hierro y el celtismo como recurso para la construcción de identidades contemporáneas en Asturias y León

El nacimiento de la Arqueología tiene una estrecha relación con el auge de los nacionalismos en toda Europa. En el estado español, tanto el nacionalismo centralista como los nacionalismos o regionalismos periféricos han utilizado referentes del pasado –a veces coincidentes– como sustento simbólico de sus narrativas. Es el caso de los celtas, pueblo mítico que ha servido tanto para afianzar la idea unitaria de España, como para refrendar la singularidad nacional/regional de territorios como Asturias y León. El papel de los arqueólogos en estos dos casos es analizado en este trabajo, pues supone una vía crucial para la reflexión historiográfica. Así, las narrativas académicas generadas en este ámbito adolecían habitualmente de una falta de crítica, que subordinaba el pasado prerromano a determinadas agendas políticas contemporáneas. La predominancia de la Historia Antigua o de visiones esencialistas, androcéntricas y socialmente conservadoras en los discursos arqueológicos caracterizan los estudios tradicionales sobre los grupos prerromanos de Asturias y León. Tras la consolidación del Estado de las Autonomías, el nacionalismo y el regionalismo se extendieron a amplias capas de la sociedad acompañados de discursos históricos que prescindieron de la legitimación de la Academia. Paradójicamente, estas narrativas reproducen discursos conservadores que tradicionalmente dominaban el discurso arqueológico. Ante esta situación, ¿nos corresponde a los arqueólogos asumir una posición multivocal liberal o deberíamos, en cambio, emprender acciones sociopolíticas críticas que inicien una autocrítica disciplinar y persigan transformar los marcos teórico-interpretativos dominantes?.

Multiwavelength study of star-forming galaxies in the local Universe

We have studied in detail the properties of local active star-forming galaxies from the UCM survey, and in particular their star-formation histories. We have quantified the relative importance of the current episode of star formation in comparison to the underlying older stellar populations. We have also determined the total stellar mass function and burst mass function for the UCM sample using the M/L calculated for each galaxy. Integrating this mass function we obtained the contribution of the star-forming galaxies to the total stellar mass density of the local Universe.

The XMM deep survey in the CDF-S. VI. Obscured AGN selected as infrared power-law galaxies

Context. Accretion onto supermassive black holes is believed to occur mostly in obscured active galactic nuclei (AGN). Such objects are proving rather elusive in surveys of distant galaxies, including those at X-ray energies. Aims. Our main goal is to determine whether the revised IRAC criteria of Donley et al. (2012, ApJ, 748, 142; objects with an infrared (IR) power-law spectral shape), are effective at selecting X-ray type-2 AGN (i.e., absorbed N_H > 10^22 cm^-2). Methods. We present the results from the X-ray spectral analysis of 147 AGN selected by cross-correlating the highest spectral quality ultra-deep XMM-Newton and the Spitzer/IRAC catalogues in the Chandra Deep Field South. Consequently it is biased towards sources with high S/N X-ray spectra. In order to measure the amount of intrinsic absorption in these sources, we adopt a simple X-ray spectral model that includes a power-law modified by intrinsic absorption at the redshift of each source and a possible soft X-ray component. Results. We find 21/147 sources to be heavily absorbed but the uncertainties in their obscuring column densities do not allow us to confirm their Compton-Thick nature without resorting to additional criteria. Although IR power-law galaxies are less numerous in our sample than IR non-power-law galaxies (60 versus 87 respectively), we find that the fraction of absorbed (N_H^intr > 10^22 cm^-2) AGN is significantly higher (at about 3 sigma level) for IR-power-law sources (similar to 2/3) than for those sources that do not meet this IR selection criteria (~1/2). This behaviour is particularly notable at low luminosities, but it appears to be present, although with a marginal significance, at all luminosities. Conclusions. We therefore conclude that the IR power-law method is efficient in finding X-ray-absorbed sources. We would then expect that the long-sought dominant population of absorbed AGN is abundant among IR power-law spectral shape sources not detected in X-rays.

Coherencia de Políticas para el Desarrollo: Propuestas para España

La ayuda al desarrollo constituye un pequeño capítulo dentro de las políticas públicas con efectos sobre los países en desarrollo. Otras políticas, como la comercial, agrícola o migratoria, por sólo citar algunas, pueden tener efectos de desarrollo de mayor entidad que la propia ayuda internacional. De poco servirá, por tanto, disponer de una política de cooperación comprometida si el resto de las decisiones que adoptan los gobiernos operan en sentido contrario. Por ello, si se quieren alcanzar logros económicos y sociales en los países más pobres, será necesario incrementar los niveles de coherencia de las políticas de los países donantes. Este propósito ha sido asumido como doctrina por la Unión Europea y la OCDE, que elaboran informes de seguimiento al respecto (UE, 2009; OCDE, 2008).

La cooperación triangular: los donantes tradicionales ante la cooperación Sur-Sur

La cooperación triangular constituye una modalidad novedosa con relevantes potencialidades para el sistema internacional de ayuda y para la cooperación española. Además de constituirse como un instrumento mediante el que impulsar la cooperación Sur-Sur, de creciente interés en la nueva arquitectura de la ayuda, le otorga a la cooperación española claras oportunidades para dar contenido práctico a la agenda con los países de renta media y, específicamente, con América Latina. Conocedora de estas implicaciones, España inició su andadura en esta modalidad de ayuda en 2005, con una actividad centrada en los países latinoamericanos. Sin embargo, no existen estudios que analicen estas intervenciones y sus implicaciones. Esto es lo que motivó un estudio promovido por la Fundación Carolina sobre dos experiencias concretas de cooperación triangular. El presente artículo presenta las principales enseñanzas extraídas de ese análisis sobre el terreno, al tiempo que recoge algunas orientaciones que puedan ser de utilidad para la práctica futura en este ámbito.

La cooperación española y la infancia. Apuntes para una redefinición estratégica

La población infantil de hoy constituye la base de la sociedad del mañana, de ahí que su bienestar actual y las oportunidades que tenga a su alcance determinarán en buena medida la senda futura de desarrollo de un país. Una consulta a los indicadores internacionales sobre la infancia revela que en los últimos años se han producido mejoras reseñables. Unos logros en los que ha influido el despliegue de un marco normativo sobre la infancia ampliamente consensuado –la Convención sobre los Derechos del Niño de 1989-, unas metas compartidas en torno a los objetivos de Desarrollo del Milenio, y una actitud más consecuente por parte de algunos países, tanto donantes como en desarrollo. No obstante, es mucho lo que resta para que las necesidades y los derechos de la infancia reciban la atención que merecen, de acuerdo con la importancia que este aspecto tiene en los procesos de desarrollo.

Integral field spectroscopy and multi-wavelength imaging of nearby spiral galaxies: NGC 5668 as a pilot case for MEGARA

MEGARA (Multi-Espectrógrafo en GTC de Alta Resolución para Astronomía) is an optical Integral-Field Unit (IFU) and Multi-Object Spectrograph (MOS) designed for the GTC 10.4 m telescope in La Palma. MEGARA will be a 3rd generation instrument for GTC. It is led by the University Complutense of Madrid with the collaboration of INAOE, IAA, UPM and comprises more than 50 researchers from a large number of institutions worldwide.

Local luminous infrared galaxies. I. Spatially resolved observations with the Spitzer infrared spectrograph

We present results from the Spitzer Infrared Spectrograph spectral mapping observations of 15 local luminous infrared galaxies (LIRGs). In this paper, we investigate the spatial variations of the mid-IR emission which includes fine structure lines, molecular hydrogen lines, polycyclic aromatic features (PAHs), continuum emission, and the 9.7 μm silicate feature. We also compare the nuclear and integrated spectra. We find that the star formation takes place in extended regions (several kpc) as probed by the PAH emission, as well as the [Ne II]12.81 μm and [Ne III]15.56 μm emissions. The behavior of the integrated PAH emission and 9.7 μm silicate feature is similar to that of local starburst galaxies. We also find that the minima of the [Ne III]15.56 μm/[Ne II]12.81 μm ratio tends to be located at the nuclei and its value is lower than that of H II regions in our LIRGs and nearby galaxies. It is likely that increased densities in the nuclei of LIRGs are responsible for the smaller nuclear [Ne III]15.56 μm/[Ne II]12.81 μm ratios. This includes the possibility that some of the most massive stars in the nuclei are still embedded in ultracompact H II regions. In a large fraction of our sample, the 11.3 μm PAH emission appears more extended than the dust 5.5 μm continuum emission. We find a dependency of the 11.3 μm PAH/7.7 μm PAH and [Ne II]12.81 μm/11.3 μm PAH ratios with the age of the stellar populations. Smaller and larger ratios, respectively, indicate recent star formation. The estimated warm (300 K

Local luminous infrared galaxies: Spatially resolved mid-infrared observations with Spitzer/IRS

Luminous Infrared (IR) Galaxies (LIRGs, L_IR=10^11-10 L_⨀) are an important cosmological class of galaxies as they are the main contributors to the co-moving star formation rate density of the universe at z=1. In this paper we present a guaranteed time observation (GTO) Spitzer InfraRed Spectrograph (IRS) program aimed to obtain spectral mapping of a sample of 14 local d<76Mpc LIRGs. The data cubes map, at least, the central 20arcsec X 20arcsec to 30 arcsec X 30 arcsec regions of the galaxies, and use all four IRS modules covering the full 5-38 μ m spectral range. The final goal of this project is to characterize fully the mid-IR properties of local LIRGs as a first step to understanding their more distant counterparts. In this paper we present the first results of this GTO program. The IRS spectral mapping data allow us to build spectral maps of the bright mid-IR emission lines (e.g., [Ne II] 12.81 μ m, [Ne III]15.56 μ m, [S III] 18.71 μ m, H_2 at 17 μ m), continuum, the 6.2 and 11.3 μ m polycyclic aromatic hydrocarbon (PAH) features, and the 9.7 μ m silicate feature, as well as to extract 1D spectra for regions of interest in each galaxy. The IRS data are used to obtain spatially resolved measurements of the extinction using the 9.7 μ m silicate feature, and to trace star forming regions using the neon lines and the PAH features. We also investigate a number of active galactic nuclei (AGN) indicators, including the presence of high excitation emission lines and a strong dust continuum emission at around 6 9.7 μ m . We finally use the integrated Spitzer/IRS spectra as templates of local LIRGs. We discuss several possible uses for these templates, including the calibration of the star formation rate of IR-bright galaxies at high redshift. We also predict the intensities of the brightest mid-IR emission lines for LIRGs as a function of redshift, and compare them with the expected sensitivities of future space IR missions.

La cooperación al desarrollo y la infancia. Apuntes estratégicos para el caso de España

El presente trabajo pretende fundamentar un enfoque estratégico para la cooperación en materia de infancia. Para ello se parte de un análisis acerca de las relaciones entre infancia y desarrollo y de un estudio comparado de los enfoques adoptados a nivel internacional. A partir de una metodología elaborada al efecto, se presenta una medición del impacto, directo e indirecto, que la ayuda española tiene en materia de infancia. Y, finalmente, se hace una propuesta de definición estratégica de la política para la infancia en el marco de los sistemas de planificación de la ayuda internacional. Aunque la medición del impacto y la propuesta estratégica se refieren a la cooperación española, la metodología de medición elaborada en este estudio y la argumentación acerca del planteamiento estratégico transcienden al caso español, pudiendo ser generalizadas a otros donantes.

Determining star formation rates for infrared galaxies

We show that measures of star formation rates (SFRs) for infrared galaxies using either single-band 24 μm or extinction-corrected Paα luminosities are consistent in the total infrared luminosity = L(TIR) ~ 10^10 L_☉ range. MIPS 24 μm photometry can yield SFRs accurately from this luminosity upward: SFR(M_☉ yr^–1) = 7.8 × 10^–10 L(24 μm, L_☉) from L(TIR) = 5× 10^9 L_☉ to 10^11 L_☉ and SFR = 7.8 × 10^–10 L(24 μm, L_☉)(7.76 × 10^–11 L(24))^0.048 for higher L(TIR). For galaxies with L(TIR) ≥ 10^10 L_☉, these new expressions should provide SFRs to within 0.2 dex. For L(TIR) ≥ 10^11 L_☉, we find that the SFR of infrared galaxies is significantly underestimated using extinction-corrected Paα (and presumably using any other optical or near-infrared recombination lines). As a part of this work, we constructed spectral energy distribution templates for eleven luminous and ultraluminous purely star forming infrared galaxies and over the spectral range 0.4 μm to 30 cm. We use these templates and the SINGS data to construct average templates from 5 μm to 30 cm for infrared galaxies with L(TIR) = 5× 10^9 to 10^13 L_☉. All of these templates are made available online.

The host galaxies and black holes of typical z~0.5-1.4 AGNs

We study the stellar and star formation properties of the host galaxies of 58 X-ray-selected AGNs in the GOODS portion of the Chandra Deep Field South (CDF-S) region at z ~ 0.5-1.4. The AGNs are selected such that their rest-frame UV to near-infrared spectral energy distributions (SEDs) are dominated by stellar emission; i.e., they show a prominent 1.6 μm bump, thus minimizing the AGN emission "contamination." This AGN population comprises approximately 50% of the X-ray-selected AGNs at these redshifts. We find that AGNs reside in the most massive galaxies at the redshifts probed here. Their characteristic stellar masses (M_* ~ 7.8 × 10^10 and M_* ~ 1.2 × 10^11 M_☉ at median redshifts of 0.67 and 1.07, respectively) appear to be representative of the X-ray-selected AGN population at these redshifts and are intermediate between those of local type 2 AGNs and high-redshift (z ~ 2) AGNs. The inferred black hole masses (M_BH ~ 2 × 10^8 M_☉) of typical AGNs are similar to those of optically identified quasars at similar redshifts. Since the AGNs in our sample are much less luminous (L_2–10 keV < 10^44 erg s^−1) than quasars, typical AGNs have low Eddington ratios (η ~ 0.01-0.001). This suggests that, at least at intermediate redshifts, the cosmic AGN "downsizing" is due to both a decrease in the characteristic stellar mass of typical host galaxies and less efficient accretion. Finally, there is no strong evidence in AGN host galaxies for either highly suppressed star formation (expected if AGNs played a role in quenching star formation) or elevated star formation when compared to mass-selected (i.e., IRAC-selected) galaxies of similar stellar masses and redshifts.

Spitzer power-law active galactic nucleus candidates in the chandra deep field-north

We define a sample of 62 galaxies in the Chandra Deep Field-North whose Spitzer IRAC SEDs exhibit the characteristic power-law emission expected of luminous AGNs. We study the multiwavelength properties of this sample and compare the AGNs selected in this way to those selected via other Spitzer color-color criteria. Only 55% of the power-law galaxies are detected in the X-ray catalog at exposures of >0.5 Ms, although a search for faint emission results in the detection of 85% of the power-law galaxies at the ≥2.5 σ detection level. Most of the remaining galaxies are likely to host AGNs that are heavily obscured in the X-ray. Because the power-law selection requires the AGNs to be energetically dominant in the near- and mid-infrared, the power-law galaxies comprise a significant fraction of the Spitzer-detected AGN population at high luminosities and redshifts. The high 24 μm detection fraction also points to a luminous population. The power-law galaxies comprise a subset of color-selected AGN candidates. A comparison with various mid-infrared color selection criteria demonstrates that while the color-selected samples contain a larger fraction of the X-ray-luminous AGNs, there is evidence that these selection techniques also suffer from a higher degree of contamination by star-forming galaxies in the deepest exposures. Considering only those power-law galaxies detected in the X-ray catalog, we derive an obscured fraction of 68% (2 : 1). Including all of the power-law galaxies suggests an obscured fraction of <81% (4 : 1).

Near-infrared and star-forming properties of local luminous infrared galaxies

We use Hubble Space Telescope (HST) NICMOS continuum and Paα observations to study the near-infrared and star formation properties of a representative sample of 30 local (d ~ 35-75 Mpc) luminous infrared galaxies (LIRGs, infrared [8-1000 μm] luminosities of log L_IR = 11-11.9 L_☉). The data provide spatial resolutions of 25-50 pc and cover the central ~3.3-7.1 kpc regions of these galaxies. About half of the LIRGs show compact (~1-2 kpc) Paα emission with a high surface brightness in the form of nuclear emission, rings, and minispirals. The rest of the sample show Paα emission along the disk and the spiral arms extending over scales of 3-7 kpc and larger. About half of the sample contains H II regions with Hα luminosities significantly higher than those observed in normal galaxies. There is a linear empirical relationship between the mid-IR 24 μm and hydrogen recombination (extinction-corrected Paα) luminosity for these LIRGs, and the H II regions in the central part of M51. This relation holds over more than four decades in luminosity, suggesting that the mid-IR emission is a good tracer of the star formation rate (SFR). Analogous to the widely used relation between the SFR and total IR luminosity of R. Kennicutt, we derive an empirical calibration of the SFR in terms of the monochromatic 24 μm luminosity that can be used for luminous, dusty galaxies.

Cuestionario de calidad de vida ULL-27: un instrumento específico para pacientes con linfedema de miembro superior tras cáncer de mama. Adaptación transcultural y validación de su versión española

En nuestro medio, el linfedema más frecuente es el que aparece en el miembro superior tras los tratamientos del cáncer de mama. Existe un interés creciente acerca de su impacto sobre la Calidad de Vida, entendida ésta como el completo estado de bienestar físico, mental y social de la persona. Para poder medir la CV en esta población, se precisan herramientas específicas, dado que los cuestionarios genéricos no recogen las particularidades de esta enfermedad. El cuestionario ULL-27 (Upper limb lymphedema) fue la primera escala específica desarrollada para valorar la calidad de vida de mujeres con linfedema de miembro superior tras cáncer de mama1. Dada la necesidad de disponer de este tipo de instrumentos en nuestro país, y habiendo mostrado el cuestionario francés ULL-27 buenas propiedades psicométricas en su estudio de validación, se planteó como objetivo su traducción al español y adaptación transcultural a nuestro medio, procediendo a continuación a su validación en una muestra de mujeres con linfedema de miembro superior tras cáncer de mama...