Costes de las inoculaciones accidentales en personal sanitario de un hospital

ResumenObjetivosEl objetivo de este estudio es calcular el coste medio a que asciende cada seguimiento de hepatitis B, C y VIH en el personal sanitario que ha sufrido una inoculación accidental, desagregar el coste en dependencia del estado serológico de la fuente e identificar los apartados que influyen en mayor grado en la cuantía de este resultado.MétodosSe realizó una descripción de costes. El programa post-exposición se modelizó en un árbol de decisión que combinaba probabilidades (porcentaje de cada tipo de fuente en función de su positividad a los tres virus e inmunización del accidentado frente a hepatitis B) y costes monetarios (pesetas del año 1994). Estos costes fueron: personal, laboratorio, farmacia, energéticos, limpieza, teléfono, material médico y de oficina, amortización y pérdidas productivas. Se realizó un análisis de sensibilidad en función del cumplimiento real del programa.ResultadosEl coste medio de cada inoculación fue de 39.564 ptas. (29.750 ptas. aplicando el análisis de sensibilidad), con un rango desde las 86.864 ptas. (fuente positiva a los tres virus y accidentado no inmunizado) a las 23.074 ptas. (fuente negativa a los tres virus). Si la fuente era hepatitis B positiva, el coste medio fue de 86.093 ptas. cuando el accidentado no estaba inmunizado y de 53.232 si lo estaba. La mayor parte del coste residió en las pruebas serológicas (rango del 72,8% al 87,7%).ConclusionesEl alto coste sugiere una evaluación adecuada del riesgo con el fin de evitar seguimientos innecesarios. El modelo utilizado permite conocer el coste de cada episodio potencialmente evitable y puede aplicarse en cualquier hospital con el objetivo de evaluar económicamente nuevos dispositivos preventivos.SummaryObjectivesThe aim of this study was to calculate the average cost of each hepatitis B, C and HIV follow-up carried out in the health personnel that have suffered an exposure to blood and body fluids and to estimate the cost for each of the different types of sources as wall as to identify the items that account for the main part of the cost.MethodsA cost analysis was carried out. The post-exposure programme was modelled in a decision tree combining probabilities (percentage of each type of source in dependence of its positivity for the three viruses and immunization state of the health personnel against hepatitis B) and monetary costs (pesetas from 1994). Costs included: salaries, laboratory, chemist, energy, cleaning, telephone, medical and office equipment, amortization and lost productivity. A sensitivity analysis was carried out with the real fulfillment of the programme.ResultsThe average cost was 39,564 ptas. (29,750 ptas. applying the sensitivity analysis), with a range from 86,864 ptas. (source positive for the three viruses and injured subject not immunized) to 23,074 ptas. (source negative for the three viruses). If the source was hepatitis B positive, the average cost was 86,093 ptas. when the injured subject was not immunized and 53,232 ptas. if he was immunized. Serologic tests account for the main part of the cost (range from 72.8% to 87.7%).ConclusionsHigh cost suggests an appropiate risk evaluation in order to avoid unnecessary follow-ups. The model used allows to know the cost of each potentially avoided episode and it could be used for any hospital in order to make an economical evaluation of new preventive devices

Azimuthal asymmetry in the risetime of the surface detector signals of the Pierre Auger Observatory

The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of development of the shower and thus provides a novel observable, $(\sec \theta)_\mathrm{max}$, sensitive to the mass composition of cosmic rays above $3 \times 10^{18}$ eV. By comparing measurements with predictions from shower simulations, we find for both of our adopted models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication that the mean cosmic-ray mass increases slowly with energy, as has been inferred from other studies. However, the mass estimates are dependent on the shower model and on the range of distance from the shower core selected. Thus the method has uncovered further deficiencies in our understanding of shower modelling that must be resolved before the mass composition can be inferred from $(\sec \theta)_\mathrm{max}$.Comment: Replaced with published version. Added journal reference and DO

The Pierre Auger Observatory: Contributions to the 34th International Cosmic Ray Conference (ICRC 2015)

Contributions of the Pierre Auger Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The NetherlandsComment: 24 proceedings, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015

Evidence for a mixed mass composition at the `ankle' in the cosmic-ray spectrum

We report a first measurement for ultra-high energy cosmic rays of the correlation between the depth of shower maximum and the signal in the water Cherenkov stations of air-showers registered simultaneously by the fluorescence and the surface detectors of the Pierre Auger Observatory. Such a correlation measurement is a unique feature of a hybrid air-shower observatory with sensitivity to both the electromagnetic and muonic components. It allows an accurate determination of the spread of primary masses in the cosmic-ray flux. Up till now, constraints on the spread of primary masses have been dominated by systematic uncertainties. The present correlation measurement is not affected by systematics in the measurement of the depth of shower maximum or the signal in the water Cherenkov stations. The analysis relies on general characteristics of air showers and is thus robust also with respect to uncertainties in hadronic event generators. The observed correlation in the energy range around the `ankle' at $\lg(E/{\rm eV})=18.5-19.0$ differs significantly from expectations for pure primary cosmic-ray compositions. A light composition made up of proton and helium only is equally inconsistent with observations. The data are explained well by a mixed composition including nuclei with mass $A > 4$. Scenarios such as the proton dip model, with almost pure compositions, are thus disfavoured as the sole explanation of the ultrahigh-energy cosmic-ray flux at Earth.Comment: Published version. Added journal reference and DOI. Added Report Numbe

Measurement of the cosmic ray spectrum above 4×10184{\times}10^{18} eV using inclined events detected with the Pierre Auger Observatory

A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-\gamma}$ with index $\gamma=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV.Comment: Replaced with published version. Added journal reference and DO

Energy Estimation of Cosmic Rays with the Engineering Radio Array of the Pierre Auger Observatory

The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal.Comment: Replaced with published version. Added journal reference and DO

Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy

We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory.Comment: Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary file