Shoulder pain prevalence in competitive swimmers: A pilot study

Objetivos: conocer la prevalencia de dolor de hombro en nadadores de competición, sus características y su relación con factores antropométricos y deportivos. Métodos: estudio de prevalencia. Ciento cuarenta nadadores/as entre 12 y 24 años cumplimentaron un cuestionario durante una fase de entrenamiento específico. Resultados: el 25,7% revelaron padecer dolor de hombro. Se hallaron relaciones estadísticamente significativas entre el dolor de hombro y episodios previos de dolor (p<0,001), experiencia superior a tres años (p=0,014), Índice de Masa Corporal (p=0,015) y la especialidad estilo (p=0,008) y distancia (p=0,011). El dolor fue significativamente más intenso durante la actividad que en reposo (p<0,001). Conclusiones: el dolor de hombro en nadadores de competición entre 12 y 24 años parece ser un problema frecuente mayor Índice de Masa Corporal y a la especialidad del nadadorObjectives: to investigate the prevalence of shoulder pain in competitive swimmers and find out the characteristics of pain as well as its relation to anthropometric and sports factors. Methods: prevalence study. A hundred and forty competitive swimmers between 12 and 24 years old completed a questionnaire in a high intensity training phase. Results: 25.7% swimmers reported shoulder pain. There were significant statistical correlations between shoulder pain and previous episodes of pain (p<0.001), more than three years of experience (p=0.014), Body Mass Index (p=0.015) and stroke (p=0.008) and distance (p=0.011) specialty. Pain was statistically correlated with activity (p<0.001). Conclusions: shoulder pain seems to be a frequent and repetitive problem in competitive swimmers between 12 and 24 years old, which increases with years of practice. Furthermore, it seems to be associated with the activity, a higher Body Mass Index and the swimmers’ specialty

The properties of the clumpy torus and BLR in the polar-scattered Seyfert 1 galaxy ESO 323-G77 through X-ray absorption variability

We report results from multi-epoch X-ray observations of the polar-scattered Seyfert 1 galaxy ESO 323-G77. The source exhibits remarkable spectral variability from months to years timescales. The observed spectral variability is entirely due to variations of the column density of a neutral absorber towards the intrinsic nuclear continuum. The column density is generally Compton-thin ranging from a few times 10$^{22}$ cm$^{-2}$ to a few times 10$^{23}$ cm$^{-2}$. However, one observation reveals a Compton-thick state with column density of the order of 1.5 $\times$ 10$^{24}$ cm$^{-2}$. The observed variability offers a rare opportunity to study the properties of the X-ray absorber(s) in an active galaxy. We identify variable X-ray absorption from two different components, namely (i) a clumpy torus whose individual clumps have a density of $\leq$ 1.7 $\times$ 10$^8$ cm$^{-3}$ and an average column density of $\sim$ 4 $\times$ 10$^{22}$ cm$^{-2}$, and (ii) the broad line region (BLR), comprising individual clouds with density of 0.1-8 $\times$ 10$^9$ cm$^{-3}$ and column density of 10$^{23}$-10$^{24}$ cm$^{-2}$. The derived properties of the clumpy torus can also be used to estimate the torus half-opening angle, which is of the order of 47 $^\circ$. We also confirm the previously reported detection of two highly ionized warm absorbers with outflow velocities of 1000-4000 km s$^{-1}$. The observed outflow velocities are consistent with the Keplerian/escape velocity at the BLR. Hence, the warm absorbers may be tentatively identified with the warm/hot inter-cloud medium which ensures that the BLR clouds are in pressure equilibrium with their surroundings. The BLR line-emitting clouds may well be the cold, dense clumps of this outflow, whose warm/hot phase is likely more homogeneous, as suggested by the lack of strong variability of the warm absorber(s) properties during our monitoring.Comment: 15 pages, 4 tables, and 9 figures. Accepted for publication in MNRA

Fossil group origins - VI. Global X-ray scaling relations of fossil galaxy clusters

We present the first pointed X-ray observations of 10 candidate fossil galaxy groups and clusters. With these Suzaku observations, we determine global temperatures and bolometric X-ray luminosities of the intracluster medium (ICM) out to $r_{500}$ for six systems in our sample. The remaining four systems show signs of significant contamination from non-ICM sources. For the six objects with successfully determined $r_{500}$ properties, we measure global temperatures in the range $2.8 \leq T_{\mathrm{X}} \leq 5.3 \ \mathrm{keV}$, bolometric X-ray luminosities of $0.8 \times 10^{44} \ \leq L_{\mathrm{X,bol}} \leq 7.7\times 10^{44} \ \mathrm{erg} \ \mathrm{s}^{-1}$, and estimate masses, as derived from $T_{\mathrm{X}}$, of $M_{500} > 10^{14} \ \mathrm{M}_{\odot}$. Fossil cluster scaling relations are constructed for a sample that combines our Suzaku observed fossils with fossils in the literature. Using measurements of global X-ray luminosity, temperature, optical luminosity, and velocity dispersion, scaling relations for the fossil sample are then compared with a control sample of non-fossil systems. We find the fits of our fossil cluster scaling relations are consistent with the relations for normal groups and clusters, indicating fossil clusters have global ICM X-ray properties similar to those of comparable mass non-fossil systems.Comment: 17 pages, 7 figures, 8 tables. Accepted for publication in MNRA

Detection of blueshifted emission and absorption and a relativistic Iron line in the X-ray spectrum of ESO 323-G077

We report on the X-ray observation of the Seyfert 1 ESO323-G077 performed with XMM-Newton. The spectra show a complex spectrum with conspicuous absorption and emission features. The continuum emission can be modelled with a power law with an index of 1.99+/-0.02 in the whole XMM-Newton energy band, marginally consistent with typical values of Type-I objects. An absorption component with an uncommonly high equivalent Hydrogen column, n_H=5.82(+0.12/-0.11)x10^22 cm-2, is affecting the soft part of the spectrum. Additionally, two warm absorption components are also present. The lower ionised one has an ionisation parameter of Log(U)=2.14(+0.06/-0.07) and an outflowing velocity of v=3200(+600/-200) km/s. Two absorption lines located at ~6.7 and ~7.0 keV can be modelled with the highly ionised absorber. The ionisation parameter and outflowing velocity of the gas measured are Log(U)=3.26(+0.19/-0.15) and v=1700(+600/-400) km/s, respectively. Four emission lines were also detected in the soft energy band. The most likely explanation for these emission lines is that they are associated with an outflowing gas with a velocity of ~2000 km/s. The data suggest that the same gas which is causing the absorption could also being responsible of these emission features. Finally, the spectrum shows the presence of a relativistic iron emission line likely originated in the accretion disc of a Kerr BH with an inclination of ~25 deg. We propose a model to explain the observed X-ray properties which invokes the presence of a two-phase outflow with cone-like structure and a velocity of the order of 2,000-4,000 km/s. The inner layer of the cone would be less ionised, or even neutral, than the outer layer. The inclination angle would be lower than the opening angle of the outflowing cone.Comment: 11 pages, accepted in MNRA

The practitioners’ perception about the use of a virtual environment as a support for the socio-educational programme Walking Family

El programa ‘Caminar en familia’ fue implementado y evaluado en el marco de un proyecto I+D a través de una metodología de investigaciónacción participativa. Se utilizó un Entorno Virtual (EV) para ofrecer un medio de apoyo a los profesionales que implementaron el programa con familias en el Sistema de Protección a la Infancia. El objetivo de estudio es evaluar un EV como herramienta para la formación, el apoyo y la gestión de datos en la implementación del programa socioeducativo ‘Caminar en familia’. Se realizó un Grupo Discusión (GD) por cada equipo de profesionales que implementó el programa en diferentes regiones de España. En total, se llevaron a cabo 10 GD con un total de 41 profesionales durante los años 2017 y 2018. Los resultados muestran que el EV se considera una bue-na herramienta para resolver dudas, acceder a los mate-riales y evaluar la implementación. Sin embargo, los pro-fesionales afirman que no se promovió la formación co-laborativa. También manifiestan que la poca disponibili-dad horaria fue una limitación para participar en el EV. Se propone para próximas investigaciones indagar en propuestas pedagógicas y tecnológicas para fomentar la formación colaborativa de profesionales durante la im-plementación de programas socioeducativosThe ‘Walking family’ programme was implemented and evaluated within the framework of a research project through a participatory action research methodology. A Virtual Environment (VE) was used to offer a means of support to the professionals who implemented the pro-gramme with families in the Child Welfare System. The aim of the study is to evaluate a VE as a tool for training, assistance and data management in the imple-mentation of the socio-educational program ‘Walk in family’. A Discussion Group (GD) was held for each team of pro-fessionals who implemented the program in different re-gions of Spain. In total, 10 GDs were carried out with a total of 41 professionals during the years 2017 and 2018. The results show that the VE is considered a good tool to solve doubts, access the materials and evaluate the im-plementation. However, professionals say that collaborative training was not promoted. They also describre that the limited time availability was a limitation to participate in the VE. It is proposed for future research to study pedagogical and technological proposals in order to encourage the collabo-rative training of professionals during the implementation of socioeducational programme

RBS1423 - a new QSO with relativistic reflection from an ionised disk

We present the analysis and results of a 20 ks XMM-Newton observation of RBS1423. X-ray spectral analysis is used to establish a significantly broadened relativistic iron K-alpha line from a highly ionised disk. A QSO at z=2.262 was considered to be the optical counterpart of this ROSAT Bright Survey X-ray source. Based on the improved XMM-Newton source position we identified a z=0.208 QSO as optical counterpart to RBS1423. The 0.2-12 keV X-ray luminosity of this radio-quiet QSO is 6x10^{44} erg/s. The XMM-EPIC spectra are well described by a power law with a significantly broadened iron K-alpha line. Disk line models for both Schwarzschild and Kerr black holes require hydrogen-like iron ions to fit the measured line profile. Significant ionisation of the reflection disk is confirmed by model fits with ionised disk models, resulting in an ionisation parameter xi~2000.Comment: 7 pages, 8 figures, accepted for publication in A&A (2 April 2007

Engulfing a radio pulsar: the case of PSR J1023+0038

The binary millisecond radio pulsar PSR J1023+0038 has been recently the subject of multiwavelength monitoring campaigns which revealed that an accretion disc has formed around the neutron star (since 2013 June). We present here the results of X-ray and UV observations carried out by the Swift satellite between 2013 October and 2014 May, and of optical and NIR observations performed with the REM telescope, the Liverpool Telescope, the 2.1-m telescope at the San Pedro M\'artir Observatory and the 1.52-m telescope at the Loiano observing station. The X-ray spectrum is well described by an absorbed power law, which is softer than the previous quiescent epoch (up to 2013 June). The strong correlation between the X-ray and the UV emissions indicates that the same mechanism should be responsible for part of the emission in these bands. Optical and infrared photometric observations show that the companion star is strongly irradiated. Double-peaked emission lines in the optical spectra provide compelling evidence for the presence of an outer accretion disc too. The spectral energy distribution from IR to X-rays is well modelled if the contributions from the companion, the disc and the intra-binary shock emission are all considered. Our extensive data set can be interpreted in terms of an engulfed radio pulsar: the radio pulsar is still active, but undetectable in the radio band due to a large amount of ionized material surrounding the compact object. X-rays and gamma-rays are produced in an intra-binary shock front between the relativistic pulsar wind and matter from the companion and an outer accretion disc. The intense spin-down power irradiates the disc and the companion star, accounting for the UV and optical emissions.Comment: 11 pages, 8 figures, 5 tables; accepted for publication on MNRA