CARACTERIZACION DE LOS PACIENTES CON SÍNDROME DEL TUNEL CARPIANO DE UN CENTRO DE SALUD EN BARRANQUILLA

OBJETIVO: Caracterizar los pacientes con STC de acuerdo a factores sociodemográficos como edad, género y ocupación. MATERIALES Y METODOS: Se realizó un estudio de tipo descriptivo en 126 pacientes con diagnóstico de síndrome del túnel del carpo, que asistieron al centro de salud Comedicosta IPS durante el año 2008. La información se recopiló de las historias clínicas de los pacientes con síndrome del túnel del carpo. RESULTADOS: El 78% de los sujetos fueron mujeres entre los 39-59 años y las actividades del hogar se identificaron como la ocupación de mayor predomino. CONCLUSIONES: Los programas para prevenir el síndrome del túnel carpiano deben tener en cuenta el género y la edad de los sujetos y aunque el síndrome se considera una enfermedad profesional, otros ámbitos como el hogar pueden determinar su presencia. ABSTRACTOBJECTIVE: Characterize patients with CTS according to demographics factors such as age, sex and occupation. MATERIALS AND METHODS: descriptive study conducted in 126 patients with diagnosis of carpal tunnel syndrome, who attended the Comedicosta IPS Health Centre during 2008. The information was collected from the medical histories of patients with carpal tunnel syndrome. RESULTS: 78% of patients are female between the age of 39-59. The activities of the home can identify as the occupation of greater dominance.CONCLUSIONS: the programmers to prevent carpal tunnel syndrome should take into account the gender and age of the subjects and although syndrome is considered an occupational disease, other areas such as home can determine its presence

Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory

The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anti-Coincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for high-energy neutrinos from the merger in the GeV–EeV energy range using the Antares, IceCube, and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within ±500 s around the merger time. Additionally, no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for high-energy neutrinos within the 14 day period following the merger, but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The non-detection is consistent with model predictions of short GRBs observed at a large off-axis angle

Multi-messenger Observations of a Binary Neutron Star Merger

International audienceOn 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of $\sim 1.7\,{\rm{s}}$ with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg(2) at a luminosity distance of ${40}_{-8}^{+8}$ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 $\,{M}_{\odot }$. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at $\sim 40\,{\rm{Mpc}}$) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position $\sim 9$ and $\sim 16$ days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta