Un día menos. Una guía epicúrea para aceptar gozosamente las cosas que no podemos cambiar

Epicuro: vida y obra. La filosofía epicúrea como sistema. Alcances y límites de la propuesta epicúrea. El pensamiento epicúreo como guía ante la sensación de finitud

Respuesta dinámica de un edificio considerando el efecto de interacción suelo-estructura

En esta monografía se presenta el análisis de un edificio de 12 niveles de elementos prefabricados en la ciudad de Ensenada donde se determina la respuesta dinámica considerando al edificio apoyado en base rígida y teniendo en cuenta el efecto de interacción suelo-estructura, en el cual se considera a la estructura apoyada en suelo blando. Se lleva a cabo un análisis lineal para evaluar la respuesta dinámica de la estructura bajo condiciones de cargas gravitacionales establecidas en un reglamento mexicano, específicamente, en el Capítulo 5 y 6 de las Normas Técnicas Complementarias sobre Criterios y Acciones para el Diseño Estructural de las Edificaciones del DF (2004). Se realiza la obtención y distribución de las fuerzas sísmicas laterales de la estructura apoyada en base rígida utilizándose los criterios de diseño y análisis estructural del Capítulo 9 de las Normas Técnicas Complementarias para Diseño por Sismo del DF (2004), que corresponden al análisis dinámico modal. La respuesta del edificio producida por el efecto de interacción suelo-estructura se determina aplicando el método mencionado en el apéndice A de estas mismas normas. Se evalúa la respuesta de sitio donde se recurre al uso de la vibración ambiental y posteriormente, mediante el método de Nakamura, se obtiene el periodo predominante del suelo necesario para estimar la relevancia del efecto de interacción suelo-estructura. En el transcurso de esta monografía, se presentan estudios de algunos autores sobre la consideración y consecuencias del efecto de interacción suelo-estructura en el análisis sísmico de edificios. Además se muestran los procedimientos a seguir para determinar la respuesta dinámica de la estructura en estudio con base rígida y considerando el efecto de interacción suelo-estructura. También se presentan las distorsiones de entrepiso, que se determinan a partir de los desplazamientos relativos de cada nivel, para la estructura con base rígida y considerando el efecto de interacción suelo-estructura. Por último se hizo la comparación de ambas distorsiones con los valores máximos permitidos de las Normas Técnicas Complementarias para Diseño por Sismo del DF (2004) establecidos en la sección 1.8 y apéndice A.4.Postprint (published version

Simulating the performance of the Southern Wide-view Gamma-ray Observatory

The Southern Wide-view Gamma-ray Observatory (SWGO) will be a next-generation gamma-ray observatory using a large array of particle detectors at a high elevation site in South America. This project is currently in a three years R&D phase in which the design will be optimised for cost and performance. Therefore it is crucial to efficiently evaluate the impact of different design options on the scientific objectives of the observatory. In this contribution, we will introduce the strategy and the simulation framework in which this evaluation takes place

The Southern Wide-field Gamma-ray Observatory reach for Primordial Black Hole evaporation

The Southern Wide-field Gamma-ray Observatory (SWGO) is a proposed ground-based gamma-ray detector that will be located in the Southern Hemisphere and is currently in its design phase. In this contribution, we will outline the prospects for Galactic science with this Observatory. Particular focus will be given to the detectability of extended sources, such as gamma-ray halos around pulsars; optimisation of the angular resolution to mitigate source confusion between known TeV sources; and studies of the energy resolution and sensitivity required to study the spectral features of PeVatrons at the highest energies. Such a facility will ideally complement contemporaneous observatories in studies of high energy astrophysical processes in our Galaxy

Benchmarking the Science for the Southern Wide-Field Gamma-ray Observatory (SWGO)

The Southern Wide-field Gamma-ray Observatory (SWGO) is the project to build a new extensive air shower particle detector for the observation of very-high-energy gamma-rays in South America. SWGO is currently planned for installation in the Southern Hemisphere, which grants it a unique science potential among ground-based gamma-ray detectors. It will complement the capabilities of CTA, working as a wide-field instrument for the monitoring of transient and variable phenomena, and will expand the sky coverage of Northern Hemisphere facilities like HAWC and LHAASO, thus granting access to the entire Galactic Plane and the Galactic Center. SWGO aims to achieve excellent sensitivity over a very large target energy range from about 100 GeV to the PeV, and improve on the performance of current sampling array instruments in all observational parameters, including energy and angular resolution, background rejection, and single-muon detection capabilities. The directives for the final observatory design will be given by a number of key science goals which are being defined over the course of the Project’s R&D phase. In this contribution we will present the core science topics and target performance goals that serve as benchmarks to guide SWGO’s design configuration

Galactic Science with the Southern Wide-field Gamma-ray Observatory

The Southern Wide-field Gamma-ray Observatory (SWGO) is a proposed ground-based gamma-ray detector that will be located in the Southern Hemisphere and is currently in its design phase. In this contribution, we will outline the prospects for Galactic science with this Observatory. Particular focus will be given to the detectability of extended sources, such as gamma-ray halos around pulsars; optimisation of the angular resolution to mitigate source confusion between known TeV sources; and studies of the energy resolution and sensitivity required to study the spectral features of PeVatrons at the highest energies. Such a facility will ideally complement contemporaneous observatories in studies of high energy astrophysical processes in our Galaxy

Monitoring Gamma-Ray Burst VHE emission with the Southern Wide-field-of-view Gamma-ray Observatory

It has been established that Gamma-Ray Bursts (GRB) can produce Very High Energy radiation (E > 100 GeV), opening a new window on the investigation of particle acceleration and radiation properties in the most energetic domain. We expect that next-generation instruments, such as the Cherenkov Telescope Array (CTA), will mark a huge improvement in their observation. However, constraints on the target visibility and the limited duty cycle of Imaging Atmospheric Cherenkov Telescopes (IACT) reduce their ability to react promptly to transient events and to characterise their general properties. Here we show that an instrument based on the Extensive Air Shower (EAS) array concept, proposed by the Southern Wide Field-of-view Gamma-ray Observatory (SWGO) Collaboration, has promising possibilities to detect and track VHE emission from GRBs. Observations made by the Fermi Large Area Telescope (Fermi-LAT) identified some events with a distinct spectral component, extending above 1 GeV or even 10 GeV, which can represent a substantial fraction of the emitted energy and also arise in early stages of the process. Using models based on these properties, we estimate the possibilities that a wide field of view and large effective area ground-based monitoring facility has to probe VHE emission from GRBs. We show that the ability to monitor VHE transients with a nearly continuous scanning of the sky grants an opportunity to access simultaneous electromagnetic counterparts to Multi-Messenger triggers up to cosmological scales, in a way that is not available to IACTs

Lake Deployment of Southern Wide-field Gamma-ray Observatory (SWGO) Detector Units

The Southern Wide-field Gamma-ray Observatory (SWGO) will be a next-generation high altitude gamma-ray survey observatory in the southern hemisphere consisting of an array of water cherenkov detectors. With its energy range, wide field of view, large duty cycle and location it will complement the other existing and planned gamma-ray observatories. In this contribution we describe the lake concept for SWGO, an alternative to a HAWC-like design with individual water tanks and a LHAASO-style design with artificial ponds. In the lake concept, bladders filled with clean water are deployed near the surface of a natural lake, where each bladder is a light-tight stand-alone unit containing one or more photosensors. We will give an overview of the advantages and challenges for this design concept and describe the first results obtained from prototyping

Double-layered Water Cherenkov Detector for SWGO

The Southern Wide-field Gamma-ray Observatory (SWGO) will use the well-established and cost-effective technique of detecting Cherenkov light produced in water-filled detection units for TeV gamma-ray astronomy. Leveraging detector material reflectivity together with an optimised aspect ratio is an option to improve the performance of an array of such detector units. The double-layered Water Cherenkov Detector units comprise chambers with single photosensors in each. A reflective upper compartment enhances sensitivity to impinging secondary particles. A shallow lower compartment enables muon tagging and consequently improves the gamma hadron separation power of the observatory. Here we present detailed studies on the double-layered unit design