Public transport accessibility model based on user experience of the urban context

Los desafíos de transporte urbano poseen importantes aspectos técnicos y geográficos, pero éstas son solo dimensiones parciales de la problemática urbana. Para diseñar sistemas de transporte que rompan con los modelos tradicionales se necesita darle un giro más humano a la movilidad, ya que todos los viajes comienzan y terminan con una distancia recorrida a pie. En tal sentido, la calidad del ambiente urbano que rodea las áreas de acceso al Transporte Público (TP) influye en la captación de pasajeros, determinando la experiencia que los usuarios tendrán en los segmentos de acceso, transición y egreso del modo elegido. Este trabajo tiene como objeto elaborar una metodología para evaluar la accesibilidad a sistemas de TP. Se presentan los resultados preliminares del desarrollo de un modelo que intenta ampliar el alcance de las herramientas existentes de análisis, al brindar un marco metodológico a escala humana y desarrollar indicadores que describan cualidades experienciales. Se propone un modelo matemático de regresión ogística de seis variables predictivas, tres de ellas se refieren a aspectos materiales del viaje y tienen en cuenta la infraestructura urbana en diferentes escalas; otras tres se refieren a la experiencia de usuario que deriva de la interacción con el ambiente construido donde se produce el viaje.Mobility and transportation challenges in globalized cities have strong technical and locational facets, but these are only partial dimensions of the problematic. In order to design transportation systems that defy conventional models, a more humane shift towards mobility is needed, understanding that every trip starts and ends with a distance traveled by foot. Within this scope, the urban environment around public transport access areas influences catchment buffer distances, determined by the user experience during the access, transition and egress segments of the trip. This research aims to elaborate a methodological framework to evaluate accessibility that widens the scope of existing analysis tools. The preliminary results of a human-scale accessibility model are presented, elaborating on descriptive indicators of experiential qualities. The Logistic Regression mathematical model used consists of six predictive variables. Three of them describe the material aspects of the trip in different urban scales and the other three account for the user experience that derives from his interaction with the surrounding environment.Fil: Barón, Gabriela N.. Consejo Nacional de Investigaciones Científicas y TécnicasFil: Allende, David G..Fil: Arena, Alejandro P.

High-Resolution Spectroscopy of the Transiting Planet Host Star TrES-1

We report on a spectroscopic determination of the stellar parameters and chemical abundances for the parent star of the transiting planet TrES-1. Based on a detailed analysis of iron lines in our Keck and Hobby-Eberly Telescope spectra, we derive Teff = 5250 ± 75 K, log g = 4.6 ± 0.2, and [Fe/H] = 0.00 ± 0.09. By measuring the Ca II activity indicator and by putting useful upper limits on the Li abundance, we constrain the age of TrES-1 to be 2.5 ± 1.5 Gyr. By comparing theoretical stellar evolution models with the observational parameters, we obtain M* = 0.89 ± 0.05 M⊙ and R* = 0.83 ± 0.05 R⊙. Our improved estimates of the stellar parameters are utilized in a new analysis of the transit photometry of TrES-1 to derive a mass Mp = (0.76 ± 0.05) MJ a radius RP = 1.04-0.05+0.08RJ, and an inclination i = 89.5-1.3+0.5 deg. The improved planetary mass and radius estimates provide the grounds for new crucial tests of theoretical models of evolution and evaporation of irradiated extrasolar giant planets

HST/STIS Optical Transit Transmission Spectra of the hot-Jupiter HD209458b

We present the transmission spectra of the hot-Jupiter HD209458b taken with the Space Telescope Imaging Spectrograph aboard the Hubble Space Telescope. Our analysis combines data at two resolutions and applies a complete pixel-by-pixel limb-darkening correction to fully reveal the spectral line shapes of atmospheric absorption features. Terrestrial-based Na I and H I contamination are identified which mask the strong exoplanetary absorption signature in the Na core, which we find reaches total absorption levels of ~0.11% in a 4.4 Ang band. The Na spectral line profile is characterized by a wide absorption profile at the lowest absorption depths, and a sharp transition to a narrow absorption profile at higher absorption values. The transmission spectra also shows the presence of an additional absorber at ~6,250 Ang, observed at both medium and low resolutions. We performed various limb-darkening tests, including using high precision limb-darkening measurements of the sun to characterize a general trend of Atlas models to slightly overestimate the amount of limb-darkening at all wavelengths, likely due to the limitations of the model's one-dimensional nature. We conclude that, despite these limitations, Atlas models can still successfully model limb-darkening in high signal-to-noise transits of solar-type stars, like HD209458, to a high level of precision over the entire optical regime (3,000-10,000 Ang) at transit phases between 2nd and 3rd contact.Comment: 18 pages, 11 figures, Accepted to Ap

Estudio de la dispersión de cenizas volcánicas del Puyehue: simulaciones y validación

El presente trabajo está centrado en la utilización y validación del modelo FALL3D para la simulación de la dispersión de aerosoles, durante la erupción del volcán Puyehue, ocurrida el 4 de junio de 2011. Este modelo Euleriano fue configurado para modelar la pluma de cenizas durante un período de 10 días. Se validaron las salidas meteorológicamente con datos de superficie y altura provenientes de estaciones de los Servicios Meteorológicos de Argentina y Chile. Asimismo, utilizando datos satelitales de MODIS, se aplicaron varios algoritmos para la detección de ceniza volcánica, verificando así la evolución de la pluma. El buen acuerdo entre las comparaciones cualitativas y cuantitativas de las simulaciones con las mediciones sugiere una adecuada aproximación de modelado y permite la aplicación futura de estas herramientas para el estudio de los efectos radiativos de aerosoles volcánicos.This work is focused on the use and validation of the Eulerian model FALL3D in the simulation of volcanic aerosol dispersion during the Puyehue volcano eruption, occurred on June 4th 2011. This Eulerian model was configured to simulate de ash plume development during a period of 10 days. Model outputs were validated against surface and upper air meteorological data obtained from the Argentina and Chile meteorological services. In addition, using MODIS satellite data, two methods for ash discrimination were applied to verify the plume evolution. The good agreement of the qualitative and quantitative comparisons between simulated and measured data suggest an appropriate modeling approach and allows a future application of these tools in the study of radiative effects of volcanic aerosols.Asociación Argentina de Energías Renovables y Medio Ambiente (ASADES

Convective Wavelength Shifts in the Spectra of Late-Type Stars

We present ultra-high resolution spectra for a set of nearby F-G-K stars on, or close to, the main sequence. The wavelength shifts of stellar lines relative to their laboratory wavelengths are measured for more than a thousand Fe I lines per star, finding a clear correlation with line depth. The observed patterns are interpreted as convective blue-shifts that become more prominent for weaker lines, which are formed in deeper atmospheric layers. A morphological sequence with spectral type or effective temperature is apparent. Two K giant stars have also been studied. The velocity span between weak and strong lines for these stars is larger than for the dwarfs and subgiants of similar spectral types. Our results show that convective wavelength shifts may seriously compromise the accuracy of absolute spectroscopic radial velocities, but that an empirical correction may be applied to measured velocities.Comment: 4 pages, 1 figure; uses emulateapj.sty; to appear in ApJ

The PuZZling Li-Rich Red Giant Associated With NGC 6819

A Li-rich red giant (RG) star (2M19411367+4003382) recently discovered in the direction of NGC 6819 belongs to the rare subset of Li-rich stars that have not yet evolved to the luminosity bump, an evolutionary stage where models predict Li can be replenished. The currently favored model to explain Li enhancement in first-ascent RGs like 2M19411367+4003382 requires deep mixing into the stellar interior. Testing this model requires a measurement of C-12/C-13, which is possible to obtain from Apache Point Observatory Galactic Evolution Experiment (APOGEE) spectra. However, the Li-rich star also has abnormal asteroseismic properties that call into question its membership in the cluster, even though its radial velocity and location on color-magnitude diagrams are consistent with membership. To address these puzzles, we have measured a wide array of abundances in the Li-rich star and three comparison stars using spectra taken as part of the APOGEE survey to determine the degree of stellar mixing, address the question of membership, and measure the surface gravity. We confirm that the Li-rich star is a RG with the same overall chemistry as the other cluster giants. However, its log g is significantly lower, consistent with the asteroseismology results and suggestive of a very low mass if the star is indeed a cluster member. Regardless of the cluster membership, the C-12/C-13 and C/N ratios of the Li-rich star are consistent with standard first dredge-up, indicating that Li dilution has already occurred, and inconsistent with internal Li enrichment scenarios that require deep mixing.National Science Foundation AST1109888NSF AST-1358862, AST 1109718, AST 1312863Alfred P. Sloan FoundationNational Science FoundationU.S. Department of Energy Office of ScienceUniversity of ArizonaBrazilian Participation GroupBrookhaven National LaboratoryCarnegie Mellon UniversityUniversity of FloridaFrench Participation GroupGerman Participation GroupHarvard UniversityInstituto de Astrofisica de CanariasMichigan State/NotreDame/JINA Participation GroupJohns Hopkins UniversityLawrence Berkeley National LaboratoryMax Planck Institute for AstrophysicsMax Planck Institute for Extraterrestrial PhysicsNew Mexico State UniversityNew York UniversityOhio State UniversityPennsylvania State UniversityUniversity of PortsmouthPrinceton UniversitySpanish Participation GroupUniversity of TokyoUniversity of UtahVanderbilt UniversityUniversity of VirginiaUniversity of WashingtonYale UniversityNational Aeronautics and Space AdministrationTwo Micron All Sky SurveyUniversity of MassachusettsInfrared Processing and Analysis Center/California Institute of TechnologyU.S. Government NAG W-2166Astronom

High-Resolution Spectroscopy of the Transiting Planet Host Star TrES-1

We report on a spectroscopic determination of the stellar parameters and chemical abundances for the parent star of the transiting planet TrES-1. Based on a detailed analysis of iron lines in our Keck and HET spectra we derive $T_\mathrm{eff} = 5250\pm 75$ K, $\log g = 4.6\pm 0.2$, and [Fe/H] $= 0.00\pm 0.09$. By measuring the \ion{Ca}{2} activity indicator and by putting useful upper limits on the Li abundance we constrain the age of TrES-1 to be $2.5\pm 1.5$ Gyr. By comparing theoretical stellar evolution models with the observational parameters we obtain $M_\star = 0.89\pm 0.05$ $M_\odot$, and $R_\star = 0.83\pm 0.05$ $R_\odot$. Our improved estimates of the stellar parameters are utilized in a new analysis of the transit photometry of TrES-1 to derive a mass $M_p = 0.76\pm 0.05$ $M_\mathrm{J}$, a radius $R_p = 1.04^{+0.08}_{-0.05}$ $R_\mathrm{J}$, and an inclination $i = 89^\circ.5^{+0.5}_{-1.3}$. The improved planetary mass and radius estimates provide the grounds for new crucial tests of theoretical models of evolution and evaporation of irradiated extrasolar giant planets.Comment: 14 pages, 3 figures, Astrophysical Journal Letters, accepte

The Spectroscopic Orbit of the Planetary Companion Transiting HD209458

We report a spectroscopic orbit with period P = 3.52433 +/- 0.00027 days for the planetary companion that transits the solar-type star HD209458. For the metallicity, mass, and radius of the star we derive [Fe/H] = 0.00 +/- 0.02, M = 1.1 +/- 0.1 solar masses, and R = 1.3 +/- 0.1 solar radii. This is based on a new analysis of the iron lines in our HIRES template spectrum, and also on the absolute magnitude and color of the star, and uses isochrones from four different sets of stellar evolution models. Using these values for the stellar parameters we reanalyze the transit data and derive an orbital inclination of i = 85.2 +/- 1.4 degrees. For the planet we derive a mass of Mp = 0.69 +/- 0.05 Jupiter masses, a radius of Rp = 1.54 +/- 0.18 Jupiter radii, and a density of 0.23 +/- 0.08 grams per cubic cm.Comment: 11 pages, 1 figure, 2 tables, LaTex, aastex, accepted for publication by ApJ Letter

Non-LTE Model Atmospheres for Late-Type Stars II. Restricted NLTE Calculations for a Solar-Like Atmosphere

We test our knowledge of the atomic opacity in the solar UV spectrum. Using the atomic data compiled in Paper I from modern, publicly available, databases, we perform calculations that are confronted with space-based observations of the Sun. At wavelengths longer than about 260 nm, LTE modeling can reproduce quite closely the observed fluxes; uncertainties in the atomic line data account fully for the differences between calculated and observed fluxes. At shorter wavelengths, departures from LTE appear to be important, as our LTE and restricted NLTE calculations differ. Analysis of visible-near infrared Na I and O I lines, two species that produce a negligible absorption in the UV, shows that observed departures from LTE for theses species can be reproduced very accurately with restricted (fixed atmospheric structure) NLTE calculations.Comment: 13 pages, 11 figures, to appear in Ap