Responsividade da escala de avaliação funcional do sentar e levantar do solo para distrofia muscular de Duchenne (FES-DMD - D4), no período de um ano

OBJETIVO: Avaliar a responsividade da escala de avaliação funcional para pacientes com distrofia muscular de Duchenne (FES-DMD-D4), sentar e levantar do solo, no período de um ano. MÉTODO: Estudo observacional, longitudinal e retrospectivo. Foi estudada, utilizando o software FES-DMDDATA, uma amostra com 25 pacientes na atividade sentar no solo e 28 pacientes para a atividade levantar do solo. As avaliações ocorreram a cada três meses no período de um ano. Para análise estatística da capacidade de resposta foram utilizados índices de tamanho de efeito, como, effect size (ES) e Standardized Response Mean (SRM). RESULTADOS: A responsividade da atividade de sentar no solo foi considerada baixa a moderada em intervalos de três meses (ES de 0.28 a 0.54 e SRM de 0.38 a 0.71), moderada a alta em intervalos de seis meses (ES de 0.69 a 1.07 e SRM de 0.86 a 1.19), alta em intervalos de nove meses (ES de 1.3 a 1.17 e SRM de 1.26 a 1.55) e doze meses (ES de 1.9 e SRM de 1.72). Na atividade levantar do solo, a responsividade variou em baixa, moderada e alta em intervalos de três meses (ES de 0.21 a 0.33 e SRM de 0.45 a 0.83), baixa a alta em intervalos de seis meses (ES de 0.46 a 0.59 e SRM de 0.73 a 0.97), moderada a alta em intervalos de nove meses (ES de 0.76 a 0.88 e SRM de 1.03 a 1.22) e alta em doze meses (ES de 1.14 e SRM de 1.25). CONCLUSÃO: Para detectar alterações clinicamente significativas e consistentes nas atividades funcionais sentar e levantar do solo recomendamos a utilização da FES-DMD-D4 em intervalos a partir de seis meses, pois foi neste período de tempo que a capacidade de resposta variou de moderada a alta

An obscured cluster associated with the H II region RCW173

Context. The discovery of several clusters of red supergiants towards l = 24°−30° has triggered interest in this area of the Galactic plane, where lines of sight are very complex and previous explorations of the stellar content were very preliminary. Aims. We attempt to characterise the stellar population associated with the H ii region RCW 173 (=Sh2-60), located at, as previous studies have suggested that this population could be beyond the Sagittarius arm. Methods. We obtained UBV photometry of a stellar field to the south of the brightest part of RCW 173, as well as spectroscopy of about twenty stars in the area. We combined our new data with archival 2MASS near-infrared photometry and Spitzer/GLIMPSE imaging and photometry, to achieve a more accurate characterisation of the stellar sources and the associated cloud. Results. We find a significant population of early-type stars located at d = 3.0 kpc, in good agreement with the “near” dynamical distance to the H ii region. This population should be located at the near intersection of the Scutum-Crux arm. A luminous O7 II star is likely to be the main source of ionisation. Many stars are concentrated around the bright nebulosity, where GLIMPSE images in the mid infrared show the presence of a bubble of excited material surrounding a cavity that coincides spatially with a number of B0-1 V stars. We interpret this as an emerging cluster, perhaps triggered by the nearby O7 II star. We also find a number of B-type giants. Some of them are located at approximately the same distance, and may be part of an older population in the same area, characterised by much lower reddening. A few have shorter distance moduli and are likely to be located in the Sagittarius arm. Conclusions. The line of sight in this direction is very complex. Optically visible tracers delineate two spiral arms, but seem to be absent beyond d ≈ 3 kpc. Several H ii regions in this area suggest that the Scutum-Crux arm contains thick clouds actively forming stars. All these populations are projected on top of the major stellar complex signposted by the clusters of red supergiants.

First EURONEAR NEA discoveries from La Palma using the INT

Since 2006, the European Near Earth Asteroids Research (EURONEAR) project has been contributing to the research of near-Earth asteroids (NEAs) within a European network. One of the main aims is the amelioration of the orbits of NEAs, and starting in 2014 February we focus on the recovery of one-opposition NEAs using the Isaac Newton Telescope (INT) in La Palma in override mode. Part of this NEA recovery project, since 2014 June EURONEAR serendipitously started to discover and secure the first NEAs from La Palma and using the INT, thanks to the teamwork including amateurs and students who promptly reduce the data, report discoveries and secure new objects recovered with the INT and few other telescopes from the EURONEAR network. Five NEAs were discovered with the INT, including 2014 LU14, 2014 NL52 (one very fast rotator), 2014 OL339 (the fourth known Earth quasi-satellite), 2014 SG143 (a quite large NEA), and 2014 VP. Another very fast moving NEA was discovered but was unfortunately lost due to lack of follow-up time. Additionally, another 14 NEA candidates were identified based on two models, all being rapidly followed-up using the INT and another 11 telescopes within the EURONEAR network. They include one object discovered by Pan-STARRS, two Mars crossers, two Hungarias, one Jupiter trojan, and other few inner main belt asteroids (MBAs). Using the INT and Sierra Nevada 1.5 m for photometry, then the Gran Telescopio de Canarias for spectroscopy, we derived the very rapid rotation of 2014 NL52, then its albedo, magnitude, size, and its spectral class. Based on the total sky coverage in dark conditions, we evaluate the actual survey discovery rate using 2-m class telescopes. One NEA is possible to be discovered randomly within minimum 2.8 deg2 and maximum 5.5 deg2. These findings update our past statistics, being based on double sky coverage and taking into account the recent increase in discovery.

Measuring the stellar wind parameters in IGR J17544-2619 and Vela X-1 constrains the accretion physics in supergiant fast X-ray transient and classical supergiant X-ray binaries

Context. Classical supergiant X-ray binaries (SGXBs) and supergiant fast X-ray transients (SFXTs) are two types of high-mass X-ray binaries (HMXBs) that present similar donors but, at the same time, show very different behavior in the X-rays. The reason for this dichotomy of wind-fed HMXBs is still a matter of debate. Among the several explanations that have been proposed, some of them invoke specific stellar wind properties of the donor stars. Only dedicated empiric analysis of the donors’ stellar wind can provide the required information to accomplish an adequate test of these theories. However, such analyses are scarce. Aims. To close this gap, we perform a comparative analysis of the optical companion in two important systems: IGR J17544-2619 (SFXT) and Vela X-1 (SGXB). We analyze the spectra of each star in detail and derive their stellar and wind properties. As a next step, we compare the wind parameters, giving us an excellent chance of recognizing key differences between donor winds in SFXTs and SGXBs. Methods. We use archival infrared, optical and ultraviolet observations, and analyze them with the non-local thermodynamic equilibrium (NLTE) Potsdam Wolf-Rayet model atmosphere code. We derive the physical properties of the stars and their stellar winds, accounting for the influence of X-rays on the stellar winds. Results. We find that the stellar parameters derived from the analysis generally agree well with the spectral types of the two donors: O9I (IGR J17544-2619) and B0.5Iae (Vela X-1). The distance to the sources have been revised and also agree well with the estimations already available in the literature. In IGR J17544-2619 we are able to narrow the uncertainty to d = 3.0 ± 0.2 kpc. From the stellar radius of the donor and its X-ray behavior, the eccentricity of IGR J17544-2619 is constrained to e< 0.25. The derived chemical abundances point to certain mixing during the lifetime of the donors. An important difference between the stellar winds of the two stars is their terminal velocities (ν∞ = 1500 km s-1 in IGR J17544-2619 and ν∞ = 700 km s-1 in Vela X-1), which have important consequences on the X-ray luminosity of these sources. Conclusions. The donors of IGR J17544-2619 and Vela X-1 have similar spectral types as well as similar parameters that physically characterize them and their spectra. In addition, the orbital parameters of the systems are similar too, with a nearly circular orbit and short orbital period. However, they show moderate differences in their stellar wind velocity and the spin period of their neutron star which has a strong impact on the X-ray luminosity of the sources. This specific combination of wind speed and pulsar spin favors an accretion regime with a persistently high luminosity in Vela X-1, while it favors an inhibiting accretion mechanism in IGR J17544-2619. Our study demonstrates that the relative wind velocity is critical in class determination for the HMXBs hosting a supergiant donor, given that it may shift the accretion mechanism from direct accretion to propeller regimes when combined with other parameters.

Bexiga hiperactiva e utilização de toxina botulínica na hiperactividade do detrusor : resultados obtidos pelo Serviço de Urologia do HSM-CHLN

Trabalho Final do Curso de Mestrado Integrado em Medicina, Faculdade de Medicina, Universidade de Lisboa, 2014

The surface brightness and colour-magnitude relations for Fornax cluster galaxies

We present BVI photometry of 190 galaxies in the central 4 x 3 deg(2) region of the Fornax cluster observed with the Michigan Curtis Schmidt Telescope. Results from the Fornax Cluster Spectroscopic Survey (FCSS) and the Flair-II Fornax Surveys have been used to confirm the membership status of galaxies in the Fornax Cluster Catalogue (FCC). In our catalogue of 213 member galaxies, 92 (43 per cent) have confirmed radial velocities. In this paper, we investigate the surface brightness-magnitude relation for Fornax cluster galaxies. Particular attention is given to the sample of cluster dwarfs and the newly discovered ultracompact dwarf galaxies (UCDs) from the FCSS. We examine the reliability of the surface brightness-magnitude relation as a method for determining cluster membership and find that at surface brightnesses fainter than 22 mag arcsec(-2), it fails in its ability to distinguish between cluster members and barely resolved background galaxies. Cluster members exhibit a strong surface brightness-magnitude relation. Both elliptical (E) galaxies and dwarf elliptical (dE) galaxies increase in surface brightness as luminosity decreases. The UCDs lie off the locus of the relation. B-V and V-I colours are determined for a sample of 113 cluster galaxies and the colour-magnitude relation is explored for each morphological type. The UCDs lie off the locus of the colour-magnitude relation. Their mean V - I colours (similar to1.09) are similar to those of globular clusters associated with NGC 1399. The location of the UCDs on both surface brightness and colour-magnitude plots supports the 'galaxy threshing' model for infalling nucleated dwarf elliptical (dE, N) galaxies.

The Hi content of compact groups of galaxies

The Hi content of Hickson Compact Groups in the southern hemisphere is measured using data from the Hi Parkes All-Sky Survey (HIPASS), and dedicated observations using the narrow band filter on the Multibeam instrument on the Parkes telescope. The expected Hi mass of these groups was estimated using the luminosity, diameter, and morphological types of the member galaxies, calibrated from published data. Taking careful account of non-detection limits, the results show that the compact group population that has been detected by these observations has an Hi content similar to that of galaxies in the reference field sample. The upper limits for the undetected groups lie within the normal range; improvement of these limits will require a large increase in sensitivity.

The HIPASS catalogue - I. Data presentation

The H I Parkes All-Sky Survey (HIPASS) catalogue forms the largest uniform catalogue of H I sources compiled to date, with 4315 sources identified purely by their H I content. The catalogue data comprise the southern region delta < + 2&DEG; of HIPASS, the first blind H I survey to cover the entire southern sky. The rms noise for this survey is 13 mJy beam(-1) and the velocity range is -1280 to 12 700 km s(-1). Data search, verification and parametrization methods are discussed along with a description of measured quantities. Full catalogue data are made available to the astronomical community including positions, velocities, velocity widths, integrated fluxes and peak flux densities. Also available are on-sky moment maps, position-velocity moment maps and spectra of catalogue sources. A number of local large-scale features are observed in the space distribution of sources, including the super-Galactic plane and the Local Void. Notably, large-scale structure is seen at low Galactic latitudes, a region normally obscured at optical wavelengths.

The HIPASS catalogue - II. Completeness reliability and parameter accuracy

The H I Parkes All Sky Survey (HIPASS) is a blind extragalactic H I 21-cm emission-line survey covering the whole southern sky from declination -90degrees to +25degrees. The HIPASS catalogue (HICAT), containing 4315 H I-selected galaxies from the region south of declination +2degrees, is presented in Meyer et al. (Paper I). This paper describes in detail the completeness and reliability of HICAT, which are calculated from the recovery rate of synthetic sources and follow-up observations, respectively. HICAT is found to be 99 per cent complete at a peak flux of 84 mJy and an integrated flux of 9.4 Jy km. s(-1). The overall reliability is 95 per cent, but rises to 99 per cent for sources with peak fluxes >58 mJy or integrated flux >8.2 Jy km s(-1). Expressions are derived for the uncertainties on the most important HICAT parameters: peak flux, integrated flux, velocity width and recessional velocity. The errors on HICAT parameters are dominated by the noise in the HIPASS data, rather than by the parametrization procedure.

Prevalence of rectocele in young nulliparous women

Background: It is generally assumed that fascial defects in the rectovaginal septum are the result of childbirth. However, rectoceles do occur in women who have never delivered vaginally. Aims: To determine the incidence of rectocele in a cohort of asymptomatic, young nulliparous women. Methods: Observational cohort study on 178 nulliparous caucasian women (aged 18-24) recruited for a twin study of pelvic floor dysfunction. All women were interviewed and examined by translabial ultrasound, supine and after voiding. In 52 women, 3D imaging was obtained and 171 datasets were complete and available for analysis. Ultrasound findings were reviewed for rectovaginal septal integrity by an assessor blinded against interview and demographic data for rectovaginal septal integrity. Results: A discontinuity of the anterior rectal wall with extrusion of rectal mucosa or contents (depth of ! 10 mm) was observed in 21/171 (12%). The depth of this herniation ranged from 10 to 25 mm and was filled with stool (n = 10) or rectal mucosa (n = 11). Defects were associated with a higher BMI (P = 0.049), with the complaint of constipation (P = 0.049) and non-significantly with straining at stool (P = 0.09). Descent of the ampulla to beyond the level of the symphysis pubis without fascial defect, that is, significant perineal relaxation, was observed in 23/171 (13%). Conclusions: Twelve percent of 171 young nulligravid caucasian women showed a defect of the rectovaginal septum. Associations were observed with higher body mass index and a history of constipation. It is hypothesised that in some women defects of the rectovaginal septum and perineal hypermobility may be congenital in nature.

Pulling out threads from the cosmic tapestry: Defining filaments of galaxies

Filaments of galaxies are the dominant feature of modern large-scale redshift surveys. They can account for up to perhaps half of the baryonic mass budget of the Universe and their distribution and abundance can help constrain cosmological models. However, there remains no single, definitive way in which to detect, describe, and define what filaments are and their extent. This work examines a number of physically motivated, as well as statistical, methods that can be used to define filaments and examines their relative merits.

The Northern HIPASS catalogue - data presentation, completeness and reliability measures

The Northern HIPASS catalogue (NHICAT) is the northern extension of the HIPASS catalogue, HICAT. This extension adds the sky area between the declination (Dec.) range of +2 degrees < delta < +25 degrees 30' to HICAT's Dec. range of -90 degrees < delta < +2 degrees. HIPASS is a blind H I survey using the Parkes Radio Telescope covering 71 per cent of the sky (including this northern extension) and a heliocentric velocity range of - 1280 to 12 700 km s(-1). The entire Virgo Cluster region has been observed in the Northern HIPASS. The galaxy catalogue, NHICAT, contains 1002 sources with nu(hel) > 300 km s(-1). Sources with -300 < nu(hel) < 300 km s(-1) were excluded to avoid contamination by Galactic emission. In total, the entire HIPASS survey has found 5317 galaxies identified purely by their HI content. The full galaxy catalogue is publicly available at http://hipass.aus-vo.org.

Quality of the written information about suicide attempters

INTRODUCTION: The aim of the study was to assess the quality of the clinical records of the patients who are seen in public hospitals in Madrid after a suicide attempt in a blind observation. METHODS: Observational, descriptive cross-sectional study conducted at four general public hospitals in Madrid (Spain). Analyses of the presence of seven indicators of information quality (previous psychiatric treatment, recent suicidal ideation, recent suicide planning behaviour, medical lethality of suicide attempt, previous suicide attempts, attitude towards the attempt, and social or family support) in 993 clinical records of 907 patients (64.5% women), ages ranging from 6 to 92 years (mean 37.1±15), admitted to hospital after a suicide attempt or who committed an attempt whilst in hospital. RESULTS: Of patients who attempted suicide, 94.9% received a psychosocial assessment. All seven indicators were documented in 22.5% of the records, whilst 23.6% recorded four or less than four indicators. Previous suicide attempts and medical lethality of current attempt were the indicators most often missed in the records. The study found no difference between the records of men and women (z=0.296; p=0.767, two tailed Mann-Whitney U test), although clinical records of patients discharged after an emergency unit intervention were more incomplete than the ones from hospitalised patients (z=2.731; p=0.006), and clinical records of repeaters were also more incomplete than the ones from non-repeaters (z=3.511; p<0.001). CONCLUSIONS: Clinical records of patients who have attempted suicide are not complete. The use of semi-structured screening instruments may improve the evaluation of patients who have self- harmed.

Fatores determinantes da near miss materna em uma unidade de terapia intensiva obstétrica: avaliação das competências profissionais da área médica

Objective: Evaluate the determinants of morbidity and mortality in an obstetric intensive care unit and professional medical skills of students/residents at a university hospital. Methods: observational cross - sectional with 492 pregnant/pue rperal women and 261 students/residents. Patients were admitted to the obstetric intensive care unit during a year, being informed about the proposals of the study and a questionnaire was applied. The analysis was performed using Microsoft Excel 2013 and G raphPad6. Chi - square tests were used to evaluate risk factors and student t test evaluates resident/students' skills concerning the cognitive test and the Mini - Cex. Results: the main risk factors to near miss were: non - white race (OR = 2.527; RR = 2.342) ; marital status(married women) (OR = 7.968; RR = 7.113) , schooling (primary) (OR = 3.177 ; RR = 2.829) , from country town (OR = 4.643 ; RR = 4.087), low income (OR = 7014 ; RR = 5.554) , gestational hypertensive disorders (OR = 16.35 ; RR = 13.27) , re alization of pre - natal (OR = 5.023 ; RR = 4.254) and C - section before labor(OR = 39.21 ; RR = 31.25). In cognitive/Mini - cex analysis were noted significant difference in the performance of students on the subject (3.75 ± 0.93, 4.03 ± 0.94 and 4.88 ± 0.35). We still observed the best performance of residents, when compared to graduation students (p < 0.01). Conclusions: the prevalence of near miss was associated with socioeconomic/clinics factors and care issues, revealing the importance of interventions to improve these indicators. In addition, we suggest a better curriculum insertion of this subject in the medical Course disciplines due the importance to avoid the near miss through of adequacy of medical education.

Periodic Breathing and Behavioral Awakenings at High Altitude.

Objectives. To study the relationship between nocturnal periodic breathing episodes and behavioral awakenings at high altitude. Methods. Observational study. It is 6-day ascent of 4 healthy subjects from Besisahar (760 meters) to Manang (3540 meters) in Nepal in March 2012. A recording pulse oximeter was worn by each subject to measure their oxygen saturation and the presence of periodic breathing continuously through the night. An actigraph was simultaneously worn in order to determine nocturnal behavioral awakenings. There were no interventions. Results. 187-hour sleep at high altitude was analyzed, and of this, 145 hours (78%) had at least one PB event. At high altitude, 10.5% (95% CI 6.5-14.6%) of total sleep time was spent in PB while 15 out of 50 awakenings (30%, 95% CI: 18-45%) occurring at high altitudes were associated with PB (P < 0.001). Conclusions. Our data reveals a higher than expected number of behavioral awakenings associated with PB compared to what would be expected by chance. This suggests that PB likely plays a role in behavioral awakenings at high altitude.