Metodología para la desagregación detallada del Lcoe de plantas fotovoltaicas a gran escala

RESUMEN: Este artículo presenta una metodología para evaluar los costos nivelados de la electricidad (Levelized Cost of Electricity) LCOE , en plantas fotovoltaicas (Photovoltaic - PV) a gran escala. Para ello se propone una desagregación detallada de los LCOE a partir de una taxonomía rigurosa que evalúa los Costos de Inversión (Investment Cost - IC )y los Gastos de Operación (Operation and Maintenance – O&M). Partiendo de la estructura de la Administración de Información Energética (Energy Information Administration – EIA) que desglosa los IC en cinco componentes, hemos añadido un nivel adicional de desagregación denominado elementos. Asimismo, una nueva estructura para desagregar los costos de O&M es presentada. La metodología es evaluada en plantas PV de 20 MW y 150 MW PV hipotéticamente ubicadas en el municipio de Uribia (Guajira Colombia). También se desarrolla un análisis de sensibilidad determinístico usando factores como el Costo Promedio Ponderado de Capital (WACC – Weighted Average Capital Cost), la energía producida, los gastos de O&M y los IC con el ánimo de facilitar las decisiones de los inversionistas.ABSTRACT: This paper presents a breakdown cost methodology to evaluate Levelized Costs of Electricity for large-scale Photovoltaic (PV) plants. The breakdown is based on a comprehensive taxonomy to evaluate Investment Costs (IC) and Operation and Maintenance (O&M) expenditures. We added an IC disaggregation level, called elements, on top of the five-component breakdown of the Energy Information Administration (EIA). In addition, a novel structure for disaggregating O&M costs is also proposed. The methodology is evaluated over a 20-MW and a 150-MW PV power plant hypothetically placed in the municipality of Uribia (Guajira Colombia). Also deterministic sensitivity analysis based on discount rate (WACC, Weighted Average Capital Cost), energy generated, O&M costs and IC is performed to aid investors in their decision

NGC 7469 as seen by MEGARA: new results from high-resolution IFU spectroscopy

We present our analysis of high-resolution (R ∼ 20 000) GTC/MEGARA integral-field unit spectroscopic observations, obtained during the commissioning run, in the inner region (12.5 arcsec × 11.3 arcsec) of the active galaxy NGC 7469, at spatial scales of 0.62 arcsec. We explore the kinematics, dynamics, ionization mechanisms, and oxygen abundances of the ionized gas, by modelling the H α-[N II] emission lines at high signal-to-noise (> 15) with multiple Gaussian components. MEGARA observations reveal, for the first time for NGC 7469, the presence of a very thin (20 pc) ionized gas disc supported by rotation (V/σ = 4.3), embedded in a thicker (222 pc), dynamically hotter (V/σ = 1.3) one. These discs nearly corotate with similar peak-to-peak velocities (163 versus 137 km s^(−1)), but with different average velocity dispersion (38 ± 1 versus 108 ± 4 km s^(−1)). The kinematics of both discs could be possibly perturbed by star-forming regions. We interpret the morphology and the kinematics of a third (broader) component (σ > 250 km s^(−1)) as suggestive of the presence of non-rotational turbulent motions possibly associated either to an outflow or to the lense. For the narrow component, the [N II]/H α ratios point to the star-formation as the dominant mechanism of ionization, being consistent with ionization from shocks in the case of the intermediate component. All components have roughly solar metallicity. In the nuclear region of NGC 7469, at r ≤ 1.85 arcsec, a very broad (FWHM = 2590 km s^(−1)) H α component is contributing (41 per cent) to the global H α-[N II] profile, being originated in the (unresolved) broad line region of the Seyfert 1.5 nucleus of NGC 7469

Spatially resolved properties of the ionized gas in the HII galaxy J084220+115000

© 2023 The Authors. We are grateful to the referee for a very thorough report that helped us improve the quality of the paper. DFA work is funded by a Consejo Nacional de Ciencia y Tecnología (CONACyT, México) grant through project A1-S22784. This publication is based on data obtained with the MEGARA instrument at the GTC, installed in the Spanish Observatorio del Roque de los Muchachos, in the island of La Palma. MEGARA has been built by a Consortium led by the Universidad Complutense de Madrid (Spain) and that also includes the Instituto de Astrofísica, Óptica y Electrónica (INAOE, México), Instituto de Astrofísica de Andalucía (CSIC, Spain), and the Universidad Politécnica de Madrid (Spain). MEGARA is funded by the Consortium institutions, GRANTECAN S.A. and European Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER 2014-2020. YDM thanks CONACYT for the research grant CB-A1-S-25070 and DRG for the research grant CB-A1-S-22784 from which the postdoctoral grant that supported DFA was obtained. RC also thanks CONACyT for the research grant CF-320152. RA acknowledges support from ANID Fondecyt Regular 1202007. ALGM acknowledges support from the Spanish Ministry of Science and Innovation, project PID2019-107408GB-C43 (ESTALLIDOS), and from Gobierno de Canarias through EU FEDER funding, project PID2020010050. JMA acknowledges the support of the Viera y Clavijo Senior program funded by ACIISI and ULL. JIP acknowledges finantial support from projects Estallidos6 AYA2016-79724-C4 (Spanish Ministerio de Economía y Competitividad), Estallidos7 PID2019-107408GB-C44 (Spanish Ministerio de Ciencia e Innovación), grant P18-FR-2664 (Junta de Andalucía), and grant SEV-2017-0709 “Center of Excellence Severo Ochoa Program” (State Agency for Research of the Spanish MCIU).We present a spatially resolved spectroscopic study for the metal poor H_(II) galaxy J084220+115000 using MEGARA Integral Field Unit observations at the Gran Telescopio Canarias. We estimated the gas metallicity using the direct method for oxygen, nitrogen and helium and found a mean value of 12+log(O/H)=8.03±0.06, and integrated electron density and temperature of ∼ 161 cm^(−3) and ∼ 15400 K, respectively. The metallicity distribution shows a large range of ∆(O/H) = 0.72 dex between the minimum and maximum (7.69±0.06 and 8.42±0.05) values, unusual in a dwarf starforming galaxy. We derived an integrated log(N/O) ratio of −1.51 ± 0.05 and found that both N/O and O/H correspond to a primary production of metals. Spatially resolved maps indicate that the gas appears to be photoionized by massive stars according to the diagnostic line ratios. Between the possible mechanisms to explain the starburst activity and the large variation of oxygen abundance in this galaxy, our data support a possible scenario where we are witnessing an ongoing interaction triggering multiple star-forming regions localized in two dominant clumps.Depto. de Física de la Tierra y AstrofísicaFac. de Ciencias FísicasTRUEConsejo Nacional de Ciencia y Tecnología (CONACyT, México)Universidad Complutense de MadridInstituto de Astrofísica, Óptica y Electrónica (INAOE, México)Instituto de Astrofísica de AndalucíaUniversidad Politécnica de MadridGRANTECAN S.AEuropean Regional Development Funds (ERDF), through Programa Operativo Canarias FEDER 2014-2020ANID Fondecyt RegularMinisterio de Ciencia e InnovaciónGobierno de Canarias through EU FEDER fundingViera y Clavijo Senior program funded by ACIISI and ULLMinisterio de Economía y Competitividad Project Estallidos6Ministerio de Economía y Competitividad Project Estallidos7Junta de Andalucía“Center of Excellence Severo Ochoa Program”pu

Relatos de comunicadores : significados culturales en torno a la comunicación indígena propia

Esta investigación busca analizar y reconocer los significados culturales de territorio e identidad que están inmersos en la comunicación propia desde la construcción dada por comunicadores que hacen parte de los procesos de comunicación indígena. El método usado es de carácter cualitativo-exploratorio con aplicación desde el campo de la psicología cultural desde un enfoque hermenéutico, y en relación con esto, se implementaron entrevistas semi-estructuradas basadas en la técnica de análisis interpretativo propuesto por Jhon B. Thompson. En los resultados, por un lado, se logra reconocer, desde la experiencia de los comunicadores, el rol de la comunicación propia indígena, vinculada los pensamientos y las particularidades culturales, dándose así un puente entre las situaciones de las comunidades y otros lugares. Por otro lado, se evidencia la relación entre la comunicación indígena y las luchas actuales por el territorio, desde la complejidad significativa de tierra y territorio que guía su forma de pensar, sentir y actuar en la comunidad. Por último, se arrojaron comprensiones en torno a la comunicación propia, siendo esta un claro referente identitario de los pueblos indígenas, así mismo como vía importante para la transmisión de identidad cultural.The purpose of this investigation is to identify the cultural meaning behind territory and identity that are immersed in the own communication process characteristic of the indigenous culture. A caulitative-exploratory method was used for the investigation with an hermeneutic focus in the field of cultural phsicology. Following this line, semi-structured interviews were used base on the interpretative analysis proposed by John B. Thompson. The results show that the role of communication that belongs to the indigenous culture links cultural particularities and thinking processes giving way for an open communication between the communities and the rest of the region. The results also showed the relationship between indigenous communication and the fight for the territory from the complexity of the significance they give their land and territory that guide the way to think, feel and act. Lastly, the importance of the comprehension of their own communication is key for the construction of their identity and an important path to transmitting their cultural identity.Psicólogo (a)Pregrad

Efectividad de la rehabilitación física en personas entre 18 a 65 años con síndrome de dolor lumbar inespecifico : una revisión sistemática

Tesis (Kinesiólogo)El dolor lumbar inespecífico es un trastorno musculoesquelético frecuente en la comunidad. Según la Organización Mundial de la Salud, el dolor lumbar inespecífico es la primera causa de consulta médica a nivel mundial (70%). Las intervenciones kinésicas presentan un sin fin de estrategias para el dolor lumbar inespecífico, pero no hay consenso sobre la efectividad terapéutica en donde se logran mejoras significativas, repercutiendo en posibles retrasos en la rehabilitación. Determinar, mediante la revisión de la literatura, exclusivamente de ensayos clínicos, qué intervención(es) del dolor lumbar inespecífico, expresa(n) en función del tiempo, cambios significativos en la disminución del dolor y mejoría de la funcionalidad en personas entre 18 a 65 años. Metodología: Para lo anterior se realizó una búsqueda en 7 bases de datos (CINAHL, Pubmed, Medline, Nursing reference center, PEDro, Central y Rehabilitation & Sports) hasta el 10/08/2016, buscando ensayos clínicos aleatorizados que cumplieran los criterios de inclusión, exclusión y calidad metodológica, siendo esta última aplicando la escala de JADAD, Oxford y la herramienta de Higgins. La búsqueda en la literatura arrojó 21 artículos que cumplieron con los criterios de selección. Estos fueron categorizados en relación al tiempo y a las similitudes del tipo de intervención que se aplicó. Conformando la lista de intervenciones que lograron una mejora estadísticamente significativa en la intensidad del dolor y la funcionalidad, se logra determinar aquellos puntos que influyen para la elección y recomendación de las intervenciones. Finalmente, a pesar de las condiciones de los diferentes artículos, se logró determinar qué categorías de intervenciones tuvieron mejoras significativas dentro de un tiempo terapéutico. Estas son, dentro de ≤ 4 semanas, “Ejercicios” y “Agentes Físicos” son extremadamente recomendables. En la etapa de 5 a 8 semanas las categorías de “Actividad Graduada”, “Terapia Manual+Ejercicios Activos” y “Ejercicios de Estabilidad Core” son favorablemente recomendable. En el periodo entre 9 a 12 semanas las categorías de “Masajes”, “Ejercicios”, “Pilates” y “Terapia Cognitiva Funcional” resultaron ser favorablemente recomendables

Spatially resolved analysis of neutralwWinds, stars, and ionized gas kinematics with MEGARA/GTC: new insights on the nearby galaxy UGC 10205

We present a comprehensive analysis of the multiphase structure of the interstellar medium (ISM) and the stellar kinematics in the edge-on nearby galaxy UGC 10205 using integral field spectroscopy (IFS) data taken with MultiEspectrógrafo en GTC de Alta Resolución para Astronomía (MEGARA) at the GTC. We explore both the neutral and the ionized gas phases using the interstellar Na I D doublet absorption (LR−V setup, R ∼ 6000) and the Hα emission line (HR−R setup, R ∼ 18000), respectively. The high-resolution data show the complexity of the Hα emission-line profile revealing the detection of up to three kinematically distinct gaseous components. Despite of this fact, a thin-disk model is able to reproduce the bulk of the ionized gas motions in the central regions of UGC 10205. The use of asymmetric drift corrections is needed to reconciliate the ionized and the stellar velocity rotation curves. We also report the detection of outflowing neutral gas material blueshifted by ∼ 87 km s^(−1) . The main physical properties that describe the observed outflow are a total mass M_(out) = (4.55 ± 0.06) × 10^(7) Mʘ and a coldgas mass outflow rate M_(out) = 0.78 0.03 Mʘ yr^(−1) . This work points out the necessity of exploiting highresolution IFS data to understand the multiphase components of the ISM and the multiple kinematical components in the central regions of nearby galaxies

MEGARA-GTC stellar spectral library: I

MEGARA (Multi Espectrografo en GTC de Alta Resolucion para Astronomia) is an optical (3650-9750 Å), fibre-fed, medium-high spectral resolution (R = 6000, 12 000 and 20 000) instrument for the Gran Telescopio CANARIAS (GTC) 10.4-m telescope, commissioned in the summer of 2017, and currently in operation. The scientific exploitation of MEGARA requires a stellar spectra library to interpret galaxy data and to estimate the contribution of the stellar populations. In this paper, we introduce the MEGARA-GTC spectral library, detailing the rationale behind the building of this catalogue. We present the spectra of 97 stars (21 individual stars and 56 members of the globular cluster M15, which are both subsamples taken during the commissioning runs, and 20 stars from our ongoing GTC Open-Time programme). The spectra have R = 20 000 in the HR-R and HR-I set-ups, centred at 6563 and 8633 Å, respectively. We describe the procedures to reduce and analyse the data. Then, we determine the best-fitting theoretical models to each spectrum through a χ^(2) minimization technique, to derive the stellar physical parameters, and we discuss the results. We have also measured some absorption lines and indices. Finally, we introduce our project to complete the library and the data base in order to make the spectra available to the community

Prevalence of Babesia Caballi, Theileria Equi and Trypanosomiasis and analysis of risk factors in horses of Antioquia, Colombia

ABSTRACT: This research was carried out due to the little existing national information on equine hemoparasites; the objective was to determine babesiosis and trypanosomiasis prevalence in the Aburrá Valley and Rionegro Antioquia (Colombia) as well as some risk factors associated with the seropositivitie of these diseases. In 223 lots with a population of 1.008 equine venous blood sample was taken for serological diagnosis and molecular. Epidemiological information was obtained through the application of a survey addressed to persons in charge of the animals. For the statistical analysis, Chi square of independence or Fisher’s Exact Test was applied when necessary. For the bivariate associations, risk estimates (OR) were calculated by explanatory variable, with their respective 95% confidence intervals (95% CI).It was found a prevalence of 11.9% for babesiosis and 1.9% for trypanosomiasis and as protection factor found the fact of going to trade fairs. Geographic location, sex and being neutered, be positive for Equine Infectious Anemia (AIE), strongyles or oxiurus was a risk factor for piroplasmosis. For Trypanosomiasis the risk factor was to be infested with ticks Dermacentor nitens or be mule. Methods of active epidemiological surveillance should be reinforced, especially in cases of continuous mobilization of equines or development of events that involve massive presence of horses.RESUMEN: La investigación se llevó a cabo debido a la poca información nacional existente en hemoparásitos equinos y su objetivo fue determinar la prevalencia de babesiosis y tripanosomiasis, en el Valle de Aburrá y Rionegro, municipios de Antioquia (Colombia), así como algunos factores de riesgo asociados a la presentación de seropositividad, a estas enfermedades. En 223 predios, con una población de 1.008 equinos, se tomó muestra de sangre venosa, para realizar el diagnóstico serológico y molecular. La información epidemiológica fue obtenida a través de la aplicación de una encuesta dirigida a las personas a cargo de los animales. Para el análisis estadístico, se aplicó Chi cuadrado de independencia y la Prueba Exacta de Fisher, cuando fue necesario. Para las asociaciones bivariadas, se calcularon estimaciones del riesgo (OR) por variable explicativa, con sus respectivos intervalos de confianza, del 95% (I.C. 95%). Se encontró una prevalencia del 11,9%, para babesiosis y de 1,9%, para tripanosomiasis; como factor de protección, se encontró el hecho de salir a una feria. Para la piroplasmosis, el lugar geográfico, el sexo, estar castrado, ser positivos a Anemia Infecciosa Equina (AIE), estrongilidos u oxiurus fueron factores de riesgo. Para tripanosomiasis, el factor de riesgo fue estar infestado con Dermacentor nitens o ser mular. Se deben reforzar métodos de vigilancia epidemiológica activa, sobre todo, en casos de movilización continua de equinos o desarrollo de eventos, que involucren presencia masiva de ejemplares

The nature of the Cygnus extreme B supergiant 2MASS J20395358+4222505

2MASS J20395358+4222505 is an obscured early B supergiant near the massive OB star association Cygnus OB2. Despite its bright infrared magnitude (Ks = 5.82) it has remained largely ignored because of its dim optical magnitude (B = 16.63, V = 13.68). In a previous paper, we classified it as a highly reddened, potentially extremely luminous, early B-type supergiant. We obtained its spectrum in the U, B and R spectral bands during commissioning observations with the instrument MEGARA at the Gran Telescopio CANARIAS. It displays a particularly strong Hα emission for its spectral type, B1 Ia. The star seems to be in an intermediate phase between supergiant and hypergiant, a group that it will probably join in the near (astronomical) future. We observe a radial velocity difference between individual observations and determine the stellar parameters, obtaining Teff = 24 000 K and log gc = 2.88 ± 0.15. The rotational velocity found is large for a B supergiant, v sin i = 110 ± 25 kms−1⁠. The abundance pattern is consistent with solar, with a mild C underabundance (based on a single line). Assuming that J20395358+4222505 is at the distance of Cyg OB2, we derive the radius from infrared photometry, finding R = 41.2 ± 4.0 R⊙, log(L/L⊙) = 5.71 ± 0.04 and a spectroscopic mass of 46.5 ± 15.0 M⊙. The clumped mass-loss rate (clumping factor 10) is very high for the spectral type, M˙ = 2.4 × 10−6 M⊙ a−1. The high rotational velocity and mass-loss rate place the star at the hot side of the bi-stability jump. Together with the nearly solar CNO abundance pattern, they may also point to evolution in a binary system, J20395358+4222505 being the initial secondary.SS-D and AH acknowledge support from the Spanish Government Ministerio de Ciencia e Innovación through grants PGC-2018-091 3741-B-C22 and CEX2019-000920-S and from the Canarian Agency for Research, Innovation and Information Society (ACIISI), of the Canary Islands Government, and the European Regional Development Fund (ERDF), under grant with reference ProID2020010016. MG and FN acknowledge financial support through Spanish grant PID2019-105552RB-C41 (MINECO/MCIU/AEI/FEDER) and from the Spanish State Research Agency (AEI) through the Unidad de Excelencia ‘María de Maeztu’-Centro de Astrobiología (CSIC-INTA) project No. MDM-2017-0737. SRB acknowledges support by the Spanish Government under grants AYA2015-68012-C2-2-P and PGC2018-093741-B-C21/C22 (MICIU/AEI/FEDER, UE). SRA acknowledges funding support from the FONDECYT Iniciación project 11171025 and the FONDECYT Regular project 1201490. JIP acknowledges finantial support from projects Estallidos6 AYA2016-79724-C4 (Spanish Ministerio de Economia y Competitividad), Estallidos7 PID2019-107408GB-C44 (Spanish Ministerio de Ciencia e Innovacion), grant P18-FR-2664 (Junta de Andalucía), and grant SEV-2017-0709 ‘Centro de Excelencia Severo Ochoa Program’ (Spanish Science Ministry). AGP, SP, AG-M, JG and NC acknowledge support from the Spanish MCI through project RTI2018-096188-B-I00