Estructura de la personalidad del menor víctima de maltrato: daños psicológicos y lesiones físicas

[ES] Se aborda la problemática del menor víctima del maltrato desde la perspectiva médica, aludiendo a las lesiones físicas y psíquicas producidas como consecuencia de este tipo de conductas. De esta forma, tras exponer una clasificación sobre las expresiones de maltrato, se profundiza en la violencia física contra el menor, los abusos sexuales y los daños psicológicos, explicando las posibles alteraciones tras este tipo de agresiones.[EU] Tratu txarrak kaltetu adingabetuen gain izaten dituzten eraginak, bai fisikoak baita psikikoak, medikuen ikuspegitik aztertzen dira. Tratu txarren eraginei buruzko zerrenda azaldu ondoren, adingabetuek jasaten duten eraso fisiko, sexual eta psikologikoen azterketa egiten da, eraso hauek ondoriotzat ekartzen dituzten gorabeherak azalduz.[FR] On aborde le problème du mineur victime du mauvais traitement du point de vue médicale, en se rérérant aux lésions physiques et psychiques produites par suite de cette sorte de conduites. De cette façon, et après un exposé de la classification des expressions des mauvais traitements, on approfondit dans la violence physique contre les mineurs, les abus sexuels et les dommages psychologiques, en expliquant les possibles altérations après cette sorte d’agressions.[EN] The problem of minors as maltreatment’s victims is tackled from a medical perspective, referring to the physical and psychical injuries caused as a result of this kind of behaviours. In this way, after classifying the different types of maltreatment, it is studied the physical violence against minors, the sexual abuse and psychological injuries, explaining the possible alterations after this kind of aggressions

The Spitzer Survey of Stellar Structure in Galaxies (S^4G): Precise Stellar Mass Distributions from Automated Dust Correction at 3.6 μm

The mid-infrared is an optimal window to trace stellar mass in nearby galaxies and the 3.6μm IRAC band has been exploited to this effect, but such mass estimates can be biased by dust emission. We present our pipeline to reveal the old stellar flux at 3.6 μm and obtain stellar mass maps for more than 1600 galaxies available from the Spitzer Survey of Stellar Structure in Galaxies (S^4G). This survey consists of images in two infrared bands (3.6 and 4.5μm), and we use the Independent Component Analysis (ICA) method presented in Meidt et al. to separate the dominant light from old stars and the dust emission that can significantly contribute to the observed 3.6μm flux. We exclude from our ICA analysis galaxies with low signal-to-noise ratio (S/N <10) and those with original [3.6]–[4.5] colors compatible with an old stellar population, indicative of little dust emission (mostly early Hubble types, which can directly provide good mass maps). For the remaining 1251 galaxies to which ICA was successfully applied, we find that as much as 10%–30% of the total light at 3.6μm typically originates from dust, and locally it can reach even higher values. This contamination fraction shows a correlation with specific star formation rates, confirming that the dust emission that we detect is related to star formation. Additionally, we have used our large sample of mass estimates to calibrate a relationship of effective mass-to-light ratio (M/L) as a function of observed [3.6]–[4.5] color:log (M/L) = -0.339(±0.057) x [3.6]-[4.5])-0.336(± 0.002). Our final pipeline products have been made public through IRSA, providing the astronomical community with an unprecedentedly large set of stellar mass maps ready to use for scientific applications

Making galaxies passive: Insights from resolved studies of nearby galaxies

The rapid suppression of star formation, or quenching, is thought to be an important process in the evolution of the most massive galaxies, but the mechanisms involved are still hotly debated. Here, we consider two agents that control star formation and can ultimately lead to its suppression: AGN feedback and galaxy mergers. In the first part of the thesis, we study the interplay between stellar structure, nuclear activity, and molecular gas in the context of AGN feeding and feedback. We start presenting our catalogue of stellar mass maps for more than 1500 nearby galaxies, which has been publicly released. Using the stellar mass map of the spiral galaxy M51, we show that there is sufficient molecular gas inflow to feed the AGN (~1 Msun/yr), and feedback effects which include a nuclear molecular outflow (at a rate comparable to the inflow), as well as a large-scale radio jet which pushes molecular gas laterally, inducing shocks and turbulence. In the second part, we address the role of galaxy mergers in the buildup of a passive population of lenticular galaxies (or S0s). While lenticulars are the most common early-type galaxies in the Universe, their formation channels remain elusive. We use numerical simulations to show that even major mergers of spiral galaxies can result in lenticulars, with a bulge-disc coupling in agreement with observations. We also find that major mergers can simultaneously account for the difference in angular momentum and concentration between spirals and S0s, as recently found by the CALIFA team. Globally, our results show that both internal processes (transport of gas and AGN feedback) and external mechanisms (mergers) have the ability to regulate and eventually suppress star formation in galaxies. Current and future instrumental advancements (ALMA, NOEMA, JWST) will permit to confirm our findings with other galaxies and further assess their relative importance

La clasificación de la OMS: Dificultades para usar un lenguaje común

La OMS adoptó en 1980 una Clasificación Internacional de Deficiencias, Discapacidades y Minusvalías (CIDDM) al objeto de delimitar claramente estos tres conceptos y crear un lenguaje internacional común. Aunque la terminología, a pesar del tiempo transcurrido, no ha sido correctameante asimilada, la OMS prepara ya una nueva clasificación que será publicada este mismo año. El autor del artículo, médico del servicio de valoración y orientación de minusvalías en Gizartekintza, analiza los motivos de la escasa utilización de la antigua terminología, destaca la confusión aún hoy imperante y presenta las principales características de la nueva clasificación

Being WISE I: Validating Stellar Population Models and M/L ratios at 3.4 and 4.6 microns

Using data from the WISE mission, we have measured near infra-red (NIR) photometry of a diverse sample of dust-free stellar systems (globular clusters, dwarf and giant early-type galaxies) which have metallicities that span the range -2.2 < [Fe/H] (dex) < 0.3. This dramatically increases the sample size and broadens the metallicity regime over which the 3.4 (W1) and 4.6 micron (W2) photometry of stellar populations have been examined. We find that the W1 - W2 colors of intermediate and old (> 2 Gyr) stellar populations are insensitive to the age of the stellar population, but that the W1 - W2 colors become bluer with increasing metallicity, a trend not well reproduced by most stellar population synthesis (SPS) models. In common with previous studies, we attribute this behavior to the increasing strength of the CO absorption feature located in the 4.6 micron bandpass with metallicity. Having used our sample to validate the efficacy of some of the SPS models, we use these models to derive stellar mass-to-light ratios in the W1 and W2 bands. Utilizing observational data from the SAURON and ATLAS3D surveys, we demonstrate that these bands provide extremely simple, yet robust stellar mass tracers for dust free older stellar populations that are freed from many of the uncertainties common among optical estimators.Comment: 11 pages, 6 figures, submitted to Ap

Validez y credibilidad del testimonio. La psicología forense experimental

[ES] La Psicología del Testimonio es una disciplina sumamente compleja cuyo campo de interés es muy amplio. Tras explicar brevemente su ámbito de estudio, se abordan tres capítulos principales: la evaluación de la mentira, la evaluación del testimonio y el testimonio del niño. La determinación de la credibilidad parece hoy en día escapar a las capacidades humanas, pero la Psicología del Testimonio ha abierto un camino en esta materia.[EU] Lekukotzaren Psikologia, gai konplexua da eta sortzen duen interesa oso zabala da. Bere ikas eremua laburki azaldu ondoren, hiru kapitulu nagusi aztertzen dira: gezurraren ebaluaketa, lekukotzaren ebaluaketa eta haurraren lekukotza. Lekukotzaren Psikologiak sinesgarritasuna zehazteko bide berri bat ireki du.[FR] La Psychologie du témoignage est une discipline extrêmement complexe dont le domaine d’intérêt est très vaste. Après expliquer brièvement son champ d’étude, on aborde trois sujets principaux: l’évaluation du mensonge, l’évaluation du témoignage et le témoignage des enfants. De nos jours la détermination de la crédibilité semble s’échapper aux capacités humaines, mais la Psychologie du Témoignage a ouvert le chemin en cette matière.[EN] The witness’ Psychology is a highly complicated doctrine which field of interest is very extensive. After a brief explanation about its field of study, three main chapters are tackled: lie’s evaluation, witness’ evaluation and children’s evidence. Nowadays the credibility’s determination seems to escape human capacities, but witness’ Psychology had opened a way in this matter

Formation of S0 galaxies through mergers. Evolution in the Tully-Fisher relation since z∼1z\sim1

(Abridged version) We explore whether a scenario that combines an origin by mergers at $z\sim$1.8-1.5 with a subsequent passive evolution of the resulting S0 remnants since $z \sim$0.8-1 is compatible with observational data of S0s in the Tully-Fisher relation (TFR). We studied a set of major and minor merger experiments from the GalMer database that generate massive S0 remnants. We analysed the location of these remnants in the photometric and stellar TFRs assuming that they correspond to $z\sim0.8$ galaxies. We then estimated their evolution in these planes over the last 7 Gyr. The results were compared with data of real S0s and spirals at different redshifts. We also tested how the use of Vcirc or Vrot,max affects the results. We found that just after $\sim$1-2 Gyr of coalescence, major mergers generate S0 remnants that are outliers of the local photometric and stellar TFRs at $z\sim0.8$. After $\sim$4-7 Gyr of passive evolution in isolation, the S0 remnants move towards the local TFR, although the initial scatter among them persists. This scatter is sensitive to the indicator used for the rotation velocity: Vcirc values yield a lower scatter than when Vrot,max values are considered instead. In the planes involving Vrot,max, a clear segregation of the S0 remnants in terms of the spin-orbit coupling of the model is observed, in which the remnants of retrograde encounters overlap with local S0s hosting counter-rotating discs. The location of the S0 remnants at $z\sim 0$ agrees well with the observed distribution of local S0 galaxies in the $\sigma_0$-$M_K$, Vcirc-$\sigma_0$ and Vrot,max-$\sigma_0$ planes. Thus, massive S0 galaxies may have been formed through major mergers that occurred at high redshift and have later evolved towards the local TFR through passive evolution in relative isolation, a mechanism that would also contribute to the scatter observed in this relation.Comment: 19 pages, 15 figures. Accepted for publication in A&