Conocimiento sobre bioseguridad con relación a actitudes y prácticas en el personal de salud, VillaEsSalud Cerro Juli enero y marzo 2021

El presente estudio tuvo como objetivo general determinar la relación entre el conocimiento, las actitudes y las prácticas sobre la bioseguridad en el personal de salud Villa ESSALUD de Cerro Juli, Arequipa. La metodología de la investigación es de tipo descriptivo relacional, en el presente estudio se empleó la técnica de observación y encuesta, como instrumento se elaboró una lista de cotejo y cuestionario, conformada por una población de 42 personas, (19 licenciados en enfermería, 15 médicos y 8 técnicos) que trabajan en Villa ESSALUD de Cerro Juli, Arequipa. Por tanto, al aplicar la prueba de correlación de Spearman, los resultados muestran que el conocimiento sobre bioseguridad está relacionado significativamente y de forma alta con las prácticas sobre las medidas de bioseguridad (p-valor = 0.000 y Rho = .0882). En tanto, el conocimiento sobre bioseguridad y las actitudes sobre bioseguridad no están relacionadas (p-valor = 0.572 y Rho = 0.090). Finalmente, se concluye que el elemento más importante de la bioseguridad en cualquier unidad prestadora de salud es el estricto cumplimiento de las prácticas y procedimientos apropiados y el uso eficiente de materiales y equipos, los que forman la primera barrera de protección para el personal de salud, el medio ambiente y los pacientes; además del abastecimiento adecuado de insumos en dichas unidades de salud y disponibles para el cumplimiento de dichas normas. Para ello el personal debe estar bien enterado y entrenado sobre las normas de bioseguridad de su unidad desalud y aplicarlas correctamente

Uso del celular y su relación con el dolor cervical en alumnos de Medicina Humana de la Universidad Nacional de Tacna 2022

Objetivo: determinar la relación entre el uso del celular y el dolor cervical en alumnos de Medicina Humana de la Universidad Nacional de Tacna, 2022. Métodos: planteamiento cuantitativo, proyección correlacional, tipo básico y diseño no experimental con una población integrada de 180 alumnos matriculados en el periodo académico 2022. Se utilizó el muestreo probabilístico aleatorio optando por 123 alumnos. Sin embargo, en el trabajo de campo se observó que el nivel de sujetos de estudio accedido fue de 147, en consecuencia, estadísticamente se utilizó dicho número. Para la recopilación de información se utilizó la metodología de la encuesta y las herramientas fueron los cuestionarios de elaboración propia basados en autores nacionales e internacionales. Resultados: se observó que del 72,1 % de veces que la variable uso del celular se expresó con un nivel regular; un 0,7 % de veces la variable dolor cervical se expresó con un nivel poco probable, un 66,7 % de casos se expresó con un nivel probable y un 4,8 % de casos se expresó con un nivel muy probable. Asimismo, la significación asintótica de correlación chi cuadrado de Pearson entre la variable uso del celular y la variable dolor cervical, posee un valor numérico de 0,000. Conclusiones: existe suficiente evidencia estadística para aceptar que existe una relación significativa entre el uso del celular y el dolor cervical en alumnos de Medicina Humana de la Universidad Nacional de Tacna, 2022

Early Science with the Large Millimeter Telescope: COOL BUDHIES I - a pilot study of molecular and atomic gas at z~0.2

An understanding of the mass build-up in galaxies over time necessitates tracing the evolution of cold gas (molecular and atomic) in galaxies. To that end, we have conducted a pilot study called CO Observations with the LMT of the Blind Ultra-Deep H I Environment Survey (COOL BUDHIES). We have observed 23 galaxies in and around the two clusters Abell 2192 (z = 0.188) and Abell 963 (z = 0.206), where 12 are cluster members and 11 are slightly in the foreground or background, using about 28 total hours on the Redshift Search Receiver (RSR) on the Large Millimeter Telescope (LMT) to measure the $^{12}$CO J = 1 --> 0 emission line and obtain molecular gas masses. These new observations provide a unique opportunity to probe both the molecular and atomic components of galaxies as a function of environment beyond the local Universe. For our sample of 23 galaxies, nine have reliable detections (S/N$\geq$3.6) of the $^{12}$CO line, and another six have marginal detections (2.0 < S/N < 3.6). For the remaining eight targets we can place upper limits on molecular gas masses roughly between $10^9$ and $10^{10} M_\odot$. Comparing our results to other studies of molecular gas, we find that our sample is significantly more abundant in molecular gas overall, when compared to the stellar and the atomic gas component, and our median molecular gas fraction lies about $1\sigma$ above the upper limits of proposed redshift evolution in earlier studies. We discuss possible reasons for this discrepancy, with the most likely conclusion being target selection and Eddington bias.Comment: MNRAS, submitte

Early Science with the Large Millimeter Telescope: Constraining the Gas Fraction of a Compact Quiescent Galaxy at z=1.883

We present constraints on the dust continuum flux and inferred gas content of a gravitationally lensed massive quiescent galaxy at $z$=1.883$\pm$0.001 using AzTEC 1.1mm imaging with the Large Millimeter Telescope. MRG-S0851 appears to be a prototypical massive compact quiescent galaxy, but has evidence that it experienced a centrally concentrated rejuvenation event in the last 100 Myr (see Akhshik et al. 2020). This galaxy is undetected in the AzTEC image but we calculate an upper limit on the millimeter flux and use this to estimate the H$_2$ mass limit via an empirically calibrated relation that assumes a constant molecular gas-to-dust ratio of 150. We constrain the 3$\sigma$ upper limit of the H$_2$ fraction from the dust continuum in MRG-S0851 to be ${M_{H_2}/M_{\star}}$ $\leq$ 6.8%. MRG-S0851 has a low gas fraction limit with a moderately low sSFR owing to the recent rejuvenation episode, which together results in a relatively short depletion time of $<$0.6 Gyr if no further H$_2$ gas is accreted. Empirical and analytical models both predict that we should have detected molecular gas in MRG-S0851, especially given the rejuvenation episode; this suggests that cold gas and/or dust is rapidly depleted in at least some early quiescent galaxies.Comment: 8 pages, 4 figures, accepted for publication in Astrophysical Journal Letters in January 2021 (in press

A Radio-to-millimeter Census of Star-forming Galaxies in Protocluster 4C~23.56 at z = 2.5 : Global and local gas kinematics

We present a study of the gas kinematics of star-forming galaxies associated with protocluster 4C 23.56 at $z=2.49$ using $0''.4$ resolution CO (4-3) data taken with ALMA. Eleven H$\alpha$ emitters (HAEs) are detected in CO (4-3), including six HAEs that were previously detected in CO (3-2) at a coarser angular resolution. The detections in both CO lines are broadly consistent in the line widths and the redshifts, confirming both detections. With an increase in the number of spectroscopic redshifts, we confirm that the protocluster is composed of two merging groups with a total halo mass of $\log{(M_{\rm cl}/M_{\odot})} =13.4-13.6$, suggesting that the protocluster would evolve into a Virgo-like cluster ($>10^{14} M_{\odot}$). We compare the CO line widths and the CO luminosities with galaxies in other (proto)clusters ($n_{\rm gal}=91$) and general fields ($n_{\rm gal}=80$) from other studies. The 4C23.56 protocluster galaxies have CO line widths and luminosities comparable to other protocluster galaxies on average. On the other hand, the CO line widths are on average broader by $\approx50\%$ compared to field galaxies, while the median CO luminosities are similar. The broader line widths can be attributed to both effects of unresolved gas-rich mergers and/or compact gas distribution, which is supported by our limited but decent angular resolution observations and the size estimate of three galaxies. Based on these results, we argue that gas-rich mergers may play a role in the retention of the specific angular momentum to a value similar to that of field populations during cluster assembly, though we need to verify this with a larger number of samples.Comment: 27 pages, 10 figures, 4 tables, ApJ in pres

Early Science with the Large Millimeter Telescope: Detection of Dust Emission in Multiple Images of a Normal Galaxy at z \u3e 4 Lensed by a Frontier Fields Cluster

We directly detect dust emission in an optically detected, multiply imaged galaxy lensed by the Frontier Fields cluster MACSJ0717.5+3745. We detect two images of the same galaxy at 1.1 mm with the AzTEC camera on the Large Millimeter Telescope leaving no ambiguity in the counterpart identification. This galaxy, MACS0717_Az9, is at z \u3e 4 and the strong lensing model (μ=7.5) allows us to calculate an intrinsic IR luminosity of 9.7 × 1010 Le and an obscured star formation rate of 14.6 ± 4.5 Me yr−1. The unobscured star formation rate from the UV is only 4.1 ± 0.3 Me yr−1, which means the total star formation rate (18.7 ± 4.5 Me yr−1) is dominated (75%–80%) by the obscured component. With an intrinsic stellar mass of only 6.9 × 109 Me, MACS0717_Az9 is one of only a handful of z \u3e 4 galaxies at these lower masses that is detected in dust emission. This galaxy lies close to the estimated star formation sequence at this epoch. However, it does not lie on the dust obscuration relation (IRX-β) for local starburst galaxies and is instead consistent with the Small Magellanic Cloud attenuation law. This remarkable lower mass galaxy, showing signs of both low metallicity and high dust content, may challenge our picture of dust production in the early universe

A Radio-to-mm Census of Star-forming Galaxies in Protocluster 4C23.56 at Z = 2.5:Gas Mass and Its Fraction Revealed with ALMA

We investigate gas contents of star-forming galaxies associated with protocluster 4C23.56 at z = 2.49 by using the redshifted CO (3-2) and 1.1 mm dust continuum with the Atacama Large Millimeter/submillimeter Array. The observations unveil seven CO detections out of 22 targeted Hα emitters (HAEs) and four out of 19 in 1.1 mm dust continuum. They have high stellar mass ({M}\star > 4× {10}10 M ⊙) and exhibit a specific star-formation rate typical of main-sequence star-forming galaxies at z˜ 2.5. Different gas-mass estimators from CO (3-2) and 1.1 mm yield consistent values for simultaneous detections. The gas mass ({M}{gas}) and gas fraction ({f}{gas}) are comparable to those of field galaxies, with {M}{gas}=[0.3,1.8]× {10}11× ({α }{CO}/(4.36× A(Z))) {M}⊙ , where {α }{CO} is the CO-to-H2 conversion factor and A(Z) is the additional correction factor for the metallicity dependence of {α }{CO}, and < {f}{gas}> =0.53+/- 0.07 from CO (3-2). Our measurements place a constraint on the cosmic gas density of high-z protoclusters, indicating that the protocluster is characterized by a gas density higher than that of the general fields by an order of magnitude. We found ρ ({H}2)˜ 5× {10}9 {M}⊙ {{Mpc}}-3 with the CO(3-2) detections. The five ALMA CO detections occur in the region of highest galaxy surface density, where the density positively correlates with global star-forming efficiency (SFE) and stellar mass. Such correlations possibly indicate a critical role of the environment on early galaxy evolution at high-z protoclusters, though future observations are necessary for confirmation