NGC922 - a New Drop-through Ring Galaxy

We have found the peculiar galaxy NGC 922 to be a new drop-through ring galaxy using multiwavelength (ultraviolet-radio) imaging and spectroscopic observations. Its 'C'-shaped morphology and tidal plume indicate a recent strong interaction with its companion which was identified with these observations. Using numerical simulations we demonstrate that the main properties of the system can be generated by a high-speed off-axis drop-through collision of a small galaxy with a larger disc system, thus making NGC 922 one of the nearest known collisional ring galaxies. While these systems are rare in the local Universe, recent deep Hubble Space Telescope images suggest they were more common in the early Universe.

An Ontology for Experimentation with a Social Simulation of Land Use Change

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Perspectiva ecológica de la actividad física : Influencia de los ambientes construidos en la actividad física comunitaria

Las estrategias para incrementar la actividad física enfatizan en políticas que propicien cambios ambientales. Las recomendaciones se basan en modelos ecológicos que describen relaciones entre conductas de salud y subsistemas interpersonales, organizacionales, comunitarios y sociales, con un abordaje interdisciplinario basado en la complejidad. El cambio de un estilo de vida rural a urbano se asocia a menos oportunidades para la actividad física y mayor riesgo de ECNT, por lo que mejoras en el diseño urbano, el transporte público, y las instalaciones recreativas, estimulan comunidades activas. El Estudio Internacional de Actividad Física y Ambientes Construidos (IPEN methods) propone una metodología común a ser aplicada en distintos países para generar insumos importantes para quienes diseñan y ejecutan políticas públicas. Se presenta el desarrollo metodológico del estudio ?Porteño?, a realizarse en la C.A.B.A., y los resultados preliminares, y no representativos, así como la discusión, del plan piloto desarrollado en el barrio de Flores, para describir la información que resulta del procesamiento y análisis de datos obtenidos a través de mediciones objetivas y subjetivas de la actividad física. Estos hallazgos informan acerca de intervenciones, basadas en la evidencia, para incrementar los niveles de actividad física, para prevenir la obesidad y las ECNT

Perspectiva ecológica de la actividad física : Influencia de los ambientes construidos en la actividad física comunitaria

Las estrategias para incrementar la actividad física enfatizan en políticas que propicien cambios ambientales. Las recomendaciones se basan en modelos ecológicos que describen relaciones entre conductas de salud y subsistemas interpersonales, organizacionales, comunitarios y sociales, con un abordaje interdisciplinario basado en la complejidad. El cambio de un estilo de vida rural a urbano se asocia a menos oportunidades para la actividad física y mayor riesgo de ECNT, por lo que mejoras en el diseño urbano, el transporte público, y las instalaciones recreativas, estimulan comunidades activas. El Estudio Internacional de Actividad Física y Ambientes Construidos (IPEN methods) propone una metodología común a ser aplicada en distintos países para generar insumos importantes para quienes diseñan y ejecutan políticas públicas. Se presenta el desarrollo metodológico del estudio ?Porteño?, a realizarse en la C.A.B.A., y los resultados preliminares, y no representativos, así como la discusión, del plan piloto desarrollado en el barrio de Flores, para describir la información que resulta del procesamiento y análisis de datos obtenidos a través de mediciones objetivas y subjetivas de la actividad física. Estos hallazgos informan acerca de intervenciones, basadas en la evidencia, para incrementar los niveles de actividad física, para prevenir la obesidad y las ECNT

The VLT-FLAMES Tarantula Survey: XVIII. Classifications and radial velocities of the B-type stars

We present spectral classifications for 438 B-type stars observed as part of the VLT-FLAMES Tarantula Survey (VFTS) in the 30 Doradus region of the Large Magellanic Cloud. Radial velocities are provided for 307 apparently single stars, and for 99 targets with radial-velocity variations which are consistent with them being spectroscopic binaries. We investigate the spatial distribution of the radial velocities across the 30 Dor region, and use the results to identify candidate runaway stars. Excluding potential runaways and members of two older clusters in the survey region (SL 639 and Hodge 301), we determine a systemic velocity for 30 Dor of 271.6 ± 12.2 km s^-1 from 273 presumed single stars. Employing a 3σ criterion we identify nine candidate runaway stars (2.9% of the single stars with radial-velocity estimates). The projected rotational velocities of the candidate runaways appear to be significantly different to those of the full B-type sample, with a strong preference for either large (≥345 km s^-1) or small (≤65 km s^-1) rotational velocities. Of the candidate runaways, VFTS 358 (classified B0.5: V) has the largest differential radial velocity (-106.9 ± 16.2 km s^-1), and a preliminary atmospheric analysis finds a significantly enriched nitrogen abundance of 12 + log (N/H) ≳ 8.5. Combined with a large rotational velocity (υ_e sin i = 345 ± 22 km s^-1), this is suggestive of past binary interaction for this star.

Perspectiva ecológica de la actividad física : Influencia de los ambientes construidos en la actividad física comunitaria

Las estrategias para incrementar la actividad física enfatizan en políticas que propicien cambios ambientales. Las recomendaciones se basan en modelos ecológicos que describen relaciones entre conductas de salud y subsistemas interpersonales, organizacionales, comunitarios y sociales, con un abordaje interdisciplinario basado en la complejidad. El cambio de un estilo de vida rural a urbano se asocia a menos oportunidades para la actividad física y mayor riesgo de ECNT, por lo que mejoras en el diseño urbano, el transporte público, y las instalaciones recreativas, estimulan comunidades activas. El Estudio Internacional de Actividad Física y Ambientes Construidos (IPEN methods) propone una metodología común a ser aplicada en distintos países para generar insumos importantes para quienes diseñan y ejecutan políticas públicas. Se presenta el desarrollo metodológico del estudio ?Porteño?, a realizarse en la C.A.B.A., y los resultados preliminares, y no representativos, así como la discusión, del plan piloto desarrollado en el barrio de Flores, para describir la información que resulta del procesamiento y análisis de datos obtenidos a través de mediciones objetivas y subjetivas de la actividad física. Estos hallazgos informan acerca de intervenciones, basadas en la evidencia, para incrementar los niveles de actividad física, para prevenir la obesidad y las ECNT

Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data

The astrophysical context in which this thesis project lies concerns the comprehension of the mutual interaction between the accretion onto a Super Massive Black Hole (SMBH) and the Star Formation (SF), that take place in the host galaxy. This is one of the key topic of the modern extragalactic astrophysical research. Indeed, it is widely accepted that to understand the physics of a galaxy, the contribution of a possible central AGN must be taken into account. The aim of this thesis is the study of the physical processes of the nearby Seyfert galaxy NGC 34. This source was selected because of the wide collection of multiwavelength data available in the literature. In addition, recently, it has been observed with the Atacama Large Submillimeter/Millimeter Array (ALMA) in Band 9. This project is divided in two main parts: first of all, we reduced and analyzed the ALMA data, obtaining the continuum and CO(6-5) maps; then, we looked for a coherent explaination of NGC 34 physical characteristics. In particular, we focused on the ISM physics, in order to understand its properties in terms of density, chemical composition and dominant radiation field (SF or accretion). This work has been done through the analysis of the spectral distribution of several CO transitions as a function of the transition number (CO SLED), obtained joining the CO(6-5) line with other transitions available in the literature. More precisely, the observed CO SLED has been compared with ISM models, including Photo-Dissociation Regions (PDRs) and X-ray-Dominated Regions (XDRs). These models have been obtained through the state-of-the-art photoionization code CLOUDY. Along with the observed CO SLED, we have taken into account other physical properties of NGC 34, such as the Star Formation Rate (SFR), the gas mass and the X-ray luminosity.

Resolved Stars' Insights into Galaxy Physics

Thesis (Ph.D.)--University of Washington, 2016-08

Traitement de données observationnelles et développement d’un code de simulation pour SpIOMM et SITELLE

L’arrivée du spectromètre imageur à transformée de Fourier SITELLE au télescope Canada-France-Hawaï souligne la nécessité d’un calculateur de temps d’exposition permettant aux utilisateurs de l’instrument de planifier leurs observations et leurs demandes de temps de télescope. Une grande partie de mon projet est ainsi le développement d’un code de simulation capable de reproduire les résultats de SITELLE et de son prédecesseur SpIOMM, installé à l’Observatoire du Mont-Mégantic. La précision des simulations est confirmée par une comparaison avec des données SpIOMM et les premières observations de SITELLE. La seconde partie de mon projet consiste en une analyse spectrale de données observationelles. Prenant avantage du grand champ de vue de SpIOMM, les caractéristiques du gaz ionisé (vitesse radiale et intensité) sont étudiées pour l’ensemble de la paire de galaxies en interaction Arp 72. La courbe de rotation dans le visible ainsi que le gradient de métallicité de NGC 5996, la galaxie principale d’Arp 72, sont obtenues ici pour la première fois. La galaxie spirale NGC 7320 est également étudiée à partir d’observations faites à la fois avec SpIOMM et SITELLE.

Nuclei of Nearby Active Galaxies: NIR and Sub-mm Views and Finalizing the LINC-NIRVANA Fringe and Flexure Tracking System: Flexure and Temperature Behavior

The work presented in my thesis addresses the two cornerstones of modern astronomy: Observation and Instrumentation. Part I deals with the observation of two nearby active galaxies, the Seyfert 2 galaxy NGC 1433 and the Seyfert 1 galaxy NGC 1566, both at a distance of $\sim10$ Mpc, which are part of the Nuclei of Galaxies (NUGA) sample. It is well established that every galaxy harbors a super massive black hole (SMBH) at its center. Furthermore, there seems to be a fundamental correlation between the stellar bulge and SMBH masses. Simulations show that massive feedback, e.g., powerful outflows, in Quasi Stellar Objects (QSOs) has an impact on the mutual growth of bulge and SMBH. Nearby galaxies follow this relation but accrete mass at much lower rates. This gives rise to the following questions: Which mechanisms allow feeding of nearby Active Galactic Nuclei (AGN)? Is this feeding triggered by events, e.g., star formation, nuclear spirals, outflows, on $\sim500$ pc scales around the AGN? Does feedback on these scales play a role in quenching the feeding process? Does it have an effect on the star formation close to the nucleus? To answer these questions I have carried out observations with the Spectrograph for INtegral Field Observation in the Near Infrared (SINFONI) at the Very Large Telescope (VLT) situated on Cerro Paranal in Chile. I have reduced and analyzed the recorded data, which contain spatial and spectral information in the H-band ($1.45 \mic-1.85 \mic$) and K-band ($1.95 \mic-2.45 \mic$) on the central $10\arcsec\times10\arcsec$ of the observed galaxies. Additionally, Atacama Large Millimeter/Sub-millimeter Array (ALMA) data at $350$ GHz ($\sim0.87$ mm) as well as optical high resolution Hubble Space Telescope (HST) images are used for the analysis. For NGC 1433 I deduce from comparison of the distributions of gas, dust, and intensity of highly ionized emission lines that the galaxy center lies $\sim70$ pc north-northwest of the prior estimate. A velocity gradient is observed at the new center, which I interpret as a bipolar outflow, a circum nuclear disk, or a combination of both. At least one dust and gas arm leads from a $r\sim200$ pc ring towards the nucleus and might feed the SMBH. Two bright warm H$_2$ gas spots are detected that indicate hidden star formation or a spiral arm-arm interaction. From the stellar velocity dispersion (SVD) I estimate a SMBH mass of $\sim1.74\times10^7$ \msol. For NGC 1566 I observe a nuclear gas disk of $\sim150$ pc in radius with a spiral structure. I estimate the total mass of this disk to be $\sim5.4\times10^7$ \msol. What mechanisms excite the gas in the disk is not clear. Neither can the existence of outflows be proven nor is star formation detected over the whole disk. On one side of the spiral structure I detect a star forming region with an estimated star formation rate of $\sim2.6\times10^{-3}$ \msol\ yr$^{-1}$. From broad Br$\gamma$ emission and SVD I estimate a mean SMBH mass of $\sim5.3\times10^6$ \msol\ with an Eddington ratio of $\sim2\times10^{-3}$. Part II deals with the final tests of the Fringe and Flexure Tracker (FFTS) for LBT INterferometric Camera and the NIR/Visible Adaptive iNterferometer for Astronomy (LINC-NIRVANA) at the Large Binocular Telescope (LBT) in Arizona, USA, which I conducted. The FFTS is the subsystem that combines the two separate beams of the LBT and enables near-infrared interferometry with a significantly large field of view. The FFTS has a cryogenic system and an ambient temperature system which are separated by the baffle system. I redesigned this baffle to guarantee the functionality of the system after the final tests in the Cologne cryostat. The redesign did not affect any scientific performance of LINC-NIRVANA. I show in the final cooldown tests that the baffle fulfills the temperature requirement and stays $<110$ K whereas the moving stages in the ambient system stay $>273$ K, which was not given for the old baffle design. Additionally, I test the tilting flexure of the whole FFTS and show that accurate positioning of the detector and the tracking during observation can be guaranteed.

Nitretação em plasma com gaiola catódica: investigação do mecanismo e estudo comparativo com a nitretação em plasma de tensão contínua

The ionic plasma nitriding is one of the most important plasma assisted treatment technique for surface modification, but it presents some inherent problems mainly in nitriding pieces with complex geometries. In the last four years has appeared a plasma nitriding technique, named ASPN (Active Screen Plasma Nitriding) in which the samples and the workload are surrounded by a metal screen on which the cathodic potential is applied. This new technique makes possible to obtain a perfect uniform nitrided layer apart from the shape of the samples. The present work is based on the development of a new nitriding plasma technique named CCPN (Cathodic Cage Plasma Nitriding) Patent PI 0603213-3 derived from ASPN, but utilizes the hollow cathode effect to increase the nitriding process efficiency. That technique has shown great improvement on the treatment of several types of steels under different process conditions, producing thicker and harder layers when compared with both, ASPN and ionic plasma nitriding, besides eliminating problems associated with the later technique. The best obtained results are due to the hollow cathode effect on the cage holes. Moreover, characteristic problems of ionic plasma nitriding are eliminated due to the fact that the luminescent discharge acts on the cage wall instead of on the samples surface, which remains under a floating potential. In this work the enhancement of the cathodic cage nitriding layers proprieties, under several conditions for some types of steels was investigated, besides the mechanism for nitrides deposition on glass substrate, concluding that the CCPN is both a diffusion and a deposition process at the same time

Reproductive performance as affected by lactation status and body fat in beef cows.

Seventy-one mature Brangus cows, 38 nonlactating (NL) and 33 in late stage of lactation (L) were fed for 192 days (Phase I) a low energy diet (L). During Phase II (65 days) 19 NL and 17 L cows were fed a high energy diet (H). The other nonlactating (19) and lactating (16) cows remained on the low energy diet. Energy restriction during Phase I did not affect (P> 0.05) cyclic ovarian activity although losses in body weight and condition were substantial. Rapid changes in body weight, condition, and percent empty body lipe (EBLP) during Phase II did not substantially influencefertility, although a five-fold difference in EBLP was observed (NL0H vs. L-L). Treatment groups did not differ (P> 0.05) in conception rate, days from the beginning of the breeding season to breeding and to conception, conception at first service, and number of services per conception. Values observed for these parameters for NL-H, L-H, NL-L, and L-L groups were respectively: 68,4%, `3,.2, 23.3, 36.8% and 1.68; 82,4% 12.7, 19.5, 58.8% and 1.29; 68.4%, 10.2, 17.4, 47.4%, and 1.41; 68.8%, 12.4, 19.5, 43.7%, and 1.50.

Desarrollo de una guía tipo IDU para la conservación y el mantenimiento de las vías del municipio de San Martín de los Llanos - Meta

89 p.

Prevalencia de punto de úlceras por presión y nivel de riesgo en el Hospital Universitario Fundación Santa Fe de Bogotá

Las úlceras por presión causadas por una presión sostenida sobre la piel y sus tejidos adyacentes es una problemática considerada de salud pública, dada su alta prevalencia, se presentan mayormente en personas que tienen restricción en su movilidad, en el 3 a 10 % de los pacientes hospitalizados; con una tasa de incidencia que oscila entre 7,7 y 26,9 %, con consecuencias para la institución por altos costos, la comunidad, el paciente y su familia. En Colombia solo se cuenta con algunos estudios en instituciones en Bogotá, Cartagena, Bucaramanga y Medellín. Los estudios de prevalencia son importantes porque permiten visualizar la situación de la problemática, incentiva la implementación de medidas preventivas y la formulación de políticas institucionales que promuevan la seguridad del paciente y la calidad de la atención. En el Hospital Universitario Fundación Santa Fe de Bogotá no se conoce con exactitud la prevalencia pero se sabe que está presente por las complicaciones y consecuencias ya mencionadas, por ende el objetivo de este estudio fue determinar la prevalencia de punto de úlceras por presión en los pacientes hospitalizados, y al finalizar ser insumo para un estudio posterior que genere un Programa de Piel Sana institucional. El estudio se realizó mediante la medición en 1 día donde se valoró todos los pacientes hospitalizados, se realizó un análisis descriptivo de cada variable, y con un análisis bivariado se obtuvo medidas de asociación para identificar la relación entre los factores de riesgo y el desarrollo de ulceras por presión.

Probing the innermost regions of AGN via time-resolved spectral analysis

The dynamics and geometry of the material inflowing and outflowing close to the supermassive black hole in active galactic nuclei are still uncertain. X-rays are the most suitable way to study the AGN innermost regions because of the Fe Kα emission line, a proxy of accretion, and Fe absorption lines produced by outflows. Winds are typically classified as Warm Absorbers (slow and mildly ionized) and Ultra Fast Outflows (fast and highly ionized). Transient Obscurers -optically thick winds that produce strong spectral hardening in X-rays, lasting from days to months- have been observed recently. Emission and absorption features vary on time-scales from hours to years, probing phenomena at different distances from the SMBH. In this work, we use time-resolved spectral analysis to investigate the accretion and ejection flows, to characterize them individually and search for correlations. We analyzed XMM-Newtomn data of a set of the brightest Seyfert 1 galaxies that went through an obscuration event: NGC 3783, NGC 3227, NGC 5548, and NGC 985. Our aim is to search for emission/absorption lines in short-duration spectra (∼ 10ks), to explore regions as close as the SMBH as the statistics allows for, and possibly catch transient phenomena. First we run a blind search to detect emission/absorption features, then we analyze their evolution with Residual Maps: we visualize simultaneously positive and negative residuals from the continuum in the time-energy plane, looking for patterns and relative time-scales. In NGC 3783 we were able to ascribe variations of the Fe Kα emission line to absorptions at the same energy due to clumps in the obscurer, whose presence is detected at >3σ, and to determine the size of the clumps. In NGC 3227 we detected a wind at ∼ 0.2c at ∼ 2σ, briefly appearing during an obscuration event.