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Amiga Nakahara, Willmott & Espeland, 2019 arnaca (Fabricius, [1777]) [Nakahara et al. (2019, ZooKeys, 821: 85-152)] = ebusa (Cramer, 1780) [Nakahara et al. (2019, ZooKeys, 821: 85-152)] = arnaea (Fabricius, 1781), missp. = aranea (Fabricius, 1793), missp. = priamis (D’Almeida, 1922) [Nakahara et al. (2019, ZooKeys, 821: 85-152)] - adela (Nakahara & Espeland, 2019) [Nakahara et al. (2019, ZooKeys, 821: 85-152)] - indianacristoi (Nakahara & Marín, 2019), stat.rev. [raised from subspecies of A. arnaca to species by Orellana et al. (2020) based on unspecified morphological differences)/Orellana et al. (2020, Anartia, 29: 54-67)/Nakahara et al. (2019, ZooKeys, 821: 85-152)] sericeella (Bates, 1854) [Nakahara & Gallardo (2020, Tropical Lepidoptera Research, 29(2): 111-114)], Published as part of Espeland, Marianne, Nakahara, Shinichi, Zacca, Thamara, Barbosa, Eduardo P., Huertas, Blanca, Marín, Mario A., Lamas, Gerardo, Benmesbah, Mohamed, Brévignon, Christian, Casagrande, Mirna M., Fåhraeus, Christer, Grishin, Nick, Kawahara, Akito Y., Mielke, Olaf H. H., Miller, Jacqueline Y., Nakamura, Ichiro, Navas, Vanessa, Patrusky, Brooke, Pyrcz, Tomasz W., Richards, Lindsay, Tan, Denise, Tyler, Stephanie, Viloria, Angel, Warren, Andrew D., Xiao, Lei, Freitas, André V. L. & Willmott, Keith R., 2023, Combining target enrichment and Sanger sequencing data to clarify the systematics of the diverse Neotropical butterfly subtribe Euptychiina (Nymphalidae, Satyrinae), pp. 1-73 in Zoological Research 2023 on page 64, DOI: 10.1111/syen.12590, http://zenodo.org/record/7909395

Cosmic rays are messengers from outer space holding the answer to the Universe's deepest mysteries: What are they exactly? Where do they come from? How do they accelerate to such energies, and how are the laws governing their interactions? At the highest energies, these unubiquitous particles can only be detected through the showers of secondary particles that they generate in their interactions with the Earth's atmosphere. Large ground-based observatories, like the Pierre Auger Observatory, detect these extensive air showers and attempt to reconstruct as much information of the primary cosmic ray as possible. In particular, the number of secondary muons is a key observable because it is directly related to the atomic mass number of the primary that generated them. Understanding the mass composition as a function of the energy would shed light on various open questions strongly linked to the origin of cosmic rays. The Pierre Auger Observatory has dedicated scintillators buried underground to directly detect muons, the Underground Muon Detector (UMD). This thesis is devoted to the accurate determination of the muon content of air showers and to the study of its composition implications. We analyze direct muon measurements of air showers with energies between $10^{17.22}\,$eV and $10^{19.46}\,$eV from two experiments. At lower energies we extensively analyze UMD data, which we complement at higher energies with measurements from the Akeno Giant Air Shower Array (AGASA). For the UMD data, we develop new methods that significantly improve the estimation of the muon number. These methods also allow for the reconstruction of the muon signal as a function of time with an unprecedented time resolution, opening the door to the reconstruction of new composition-sensitive observables. As a direct application, we study the measured lateral distribution of muons and the models that attempt to describe it. Furthermore, we analyze the mass composition implications of the UMD and AGASA data. The composition interpretation of the data can only be inferred by a comparison against air-shower simulations. We therefore simulate single-proton, single-iron, and mixed composition scenarios based on the three newest-generation high-energy hadronic interaction models. To better compare the results against those of other experiments, we compute the so called $z$-values, a scale of the muon content in data relative to that of proton and iron simulations. The combined results offer a picture consistent with other experiments: the unexpectedly heavy composition constitutes evidence of a muon deficit in air-shower simulations that increases with the energy. These results can help to improve the high-energy hadronic interaction models, which in turn would improve the precision of the inferred mass composition.

This paper reports part of the experiences of the UFSC extension project entitled “Community Garden and Environmental Education in Morro do Horacio”, carried out at the Beneficent Educational and Assistance Association Gente Amiga (Florianopolis/SC), between 2018 and 2020. Among the activities developed, highlights to the implementation of a community vegetable garden, actions of Agroecology, Permaculture and Environmental Education with the children and adolescents served by the Association and with the community in general. It was noted the importance of acknowledgement, approximation and exchange of popular and academic knowledge, reinforcing the commitment of the University to adjacent communities and the role of the university extension.

The last book by the Chilean writer Pedro Lemebel (1952–2015) is entitled Mi Amiga Gladys (2016), a production entirely dedicated to his friend Gladys Marín (1938–2005). To date, this work has attracted little attention from academia, perhaps due to its apparently less confrontational discourse, one of the common characteristics of Lemebel’s previous works. However, this essay proposes that Lemebel’s last book in fact reveals a political statement, yet disguised as an intimate/sensitive declaration. This element would reflect a literary strategy employed by the writer, possibly aiming at eliciting a sympathetic response from the reader, by appealing to his/her emotions. By drawing on Affect theory, this essay argues that Lemebel’s personal/emotional stories with Gladys aim at recuperating her legacy, highlighting his friend’s social commitment and spirit of resistance. His contribution is indeed relevant to Chilean culture, as Lemebel views Chile’s recent past, so arguably conflicted and fragmented in its post-dictatorship period (from 1990 onwards). This study aims at being an innovative contribution to Lemebel’s studies, as it approaches his political discourse from an affective perspective, possibly establishing an original model for future analyses of his work.

This article aims to discuss the role of “disk magazines” in the identity construction and performance of masculinity among Polish adolescents. It examines the subculture of users of popular home computers Commodore 64 and Commodore Amiga during the post-communist system transition. Both written content and visual form were used by disk magazine editors to manifest their position in the peer group and perform their masculinity. This article outlines how youth actively constructed cultural forms and meanings that reflect the outside world both in terms of mass media culture and the ongoing process of post-communist transition.

For its enthusiasts, the blockchain is an archivist's dream come true: an immutable historical record that is publicly accessible and immune from censorship. Proposals like Juried Protocol Galleries could enable bots to compute the provenance of digital artworks and their appearance in exhibitions and publications. Distributed file systems like IPFS claim to store creative works in a redundant, networked fashion outside the control of any single cloud provider. Projects designed to work with blockchains like Filecoin and Arweave propose a dedicated cryptocurrency as financial incentive to support the cost of governing and sustaining this "permaweb." As dreamy as this picture sounds, many of these promises depend on technologies that have yet to be sufficiently developed or adopted. Rather than forecast the future, we can separate the hype from the reality in the present day by examining a real-life example, namely the 2021 auction of Andy Warhol's digital art with NFTs. This essay will focus less on blockchain's general promise as a preservation medium and more on the particular case of the digital Warhols, which both in form and spirit would seem a perfect application of NFTs to preserve historically important works of digital art. Which promises of the crypto-dream of permanent access to digital heritage ring true for this case study, and which are overblown?

The Auger Muons and Infill for the Ground Array (AMIGA) is an enhancement of the Pierre Auger Observatory, whose purpose is to lower the energy threshold of the observatory down to 10$^{16.5}$ eV, and to measure the muonic content of air showers directly. These measurements will significantly contribute to the determination of primary particle masses in the range between the second knee and the ankle, to the study of hadronic interaction models with air showers, and, in turn, to the understanding of the muon puzzle. The underground muon detector of AMIGA is concomitant to two triangular grids of water-Cherenkov stations with spacings of 433 and 750 m; each grid position is equipped with a 30\,m$^2$ plastic scintillator buried at 2.3 m depth. After the engineering array completion in early 2018 and general improvements to the design, the production phase commenced. In this work, we report on the status of the underground muon detector, the progress of its deployment, and the performance achieved after two years of operation. The detector construction is foreseen to finish by mid-2022.

We present a detailed description of the simulation development and validation of the underground muon detector signal for the Pierre Auger Observatory. To this aim, the detection system was thoroughly characterized in the laboratory. It consists of plastic-scintillator strips with optical fibers that conduct light towards silicon photomultipliers whose output is then processed with two complementary read-out channels. These measurements allowed us to design a fast and reliable simulation chain that fully reproduces the signal of single muons impinging on the scintillators.

[ES] Mediante el desarrollo de este trabajo, se establece el contexto histórico y la influencia en la informática doméstica de los microordenadores Commodore desde mitad de los años 70 hasta que desaparece la empresa a mediados de los años 90, exponiendo los distintos lanzamientos de ordenadores y las etapas por las que pasa la empresa Commodore. También se analizan los modelos más relevantes de microordenadores Commodore, detallando las características técnicas de cada uno y destacando sus particularidades respecto al resto de ordenadores, remarcando especialmente el modelo Commodore 64 por el papel que jugó en la industria de la informática. Además, este trabajo recopila diversos recursos relacionados con estos microordenadores, como los videojuegos más destacados, las distintas revistas y anuncios que ayudaron a extender su popularidad o diversos recursos y emuladores disponibles en internet. Por último se describe el lenguaje de programación BASIC que utilizan estos ordenadores y se desarrollan unos programas BASIC para mostrar su funcionamiento, comparándolos con lenguajes más modernos, como Python. Junto con estos programas, también se expone una serie de benchmarks con los que medir el rendimiento de este lenguaje en los microordenadores. Como parte de este trabajo, también se ha desarrollado una página web con finalidad divulgativa sobre los ordenadores Commodore para el Museo de Informática de la ETSINF., [EN] Through the development of this work, the historical context and the influence on home computing of Commodore microcomputers from the mid-70s until the company disappeared in the mid-90s is established, exposing the different computer launches and stages the Commodore company goes through. The most relevant models of Commodore microcomputers are also analyzed, detailing the technical characteristics of each one and highlighting their particularities compared to other computers, especially highlighting the Commodore 64 model for the role it played in the computer industry. In addition, this work compiles various resources related to these microcomputers, such as the most prominent video games, the different magazines and advertisements that helped spread their popularity or various resources and emulators available on the internet. Finally, the BASIC programming language used by these computers is described and some BASIC programs are developed to show its operation, comparing them with more modern languages, such as Python. Along with these programs, a series of benchmarks are also exposed with which to measure the performance of this language in microcomputers. As part of this work, a web page has also been developed with an informative purpose on Commodore computers for the ETSINF Computer Museum., [CA] Mitjançant el desenvolupament d’aquest treball, s’estableix el context històric i la influència en la informàtica domèstica dels microordinadors Commodore des de meitat dels anys 70 fins que desapareix l’empresa a mitjan anys 90, exposant els diferents llançaments d’ordinadors i les etapes per les quals passa l’empresa Commodore. També s’analitzen els models més rellevants de microordinadors Commodore, detallant les característiques tècniques de cadascun i destacant les seues particularitats respecte a la resta d’ordinadors, remarcant especialment el model Commodore 64 pel paper que va jugar en la indústria de la informàtica. A més, aquest treball recopila diversos recursos relacionats amb aquests microordinadors, com els videojocs més destacats, les diferents revistes i anuncis que van ajudar a estendre la seua popularitat o diversos recursos i emuladors disponibles en internet. Finalment es descriu el llenguatge de programació BASIC que utilitzen aquests ordinadors i es desenvolupen uns programes BASIC per a mostrar el seu funcionament, comparant-los amb llenguatges més moderns, com Python. Juntament amb aquests programes, també s’exposa una sèrie de benchmarks amb els quals mesurar el rendiment d’aquest llenguatge en els microordinadors. Com a part d’aquest treball, també s’ha desenvolupat una pàgina web amb finalitat divulgativa sobre els ordinadors Commodore per al Museu d’Informàtica de l’ETSINF.

The analysis of microbial growth is one of the central methods in the field of microbiology. Microbial growth dynamics can be characterized by growth parameters including carrying capacity, exponential growth rate, and growth lag. However, growth assays with clinical isolates, fastidious organisms, or microbes under stress often produce atypical growth shapes that do not follow the classical microbial growth pattern. Here, we introduce the Analysis of Microbial Growth Assays (AMiGA) software which streamlines the analysis of growth curves without any assumptions about their shapes. AMiGA can pool replicates of growth curves and infer summary statistics for biologically meaningful growth parameters. In addition, AMiGA can quantify death phases and characterize diauxic shifts. It can also statistically test for differential growth under distinct experimental conditions. Altogether, AMiGA streamlines the organization, analysis, and visualization of microbial growth assays.IMPORTANCEOur current understanding of microbial physiology relies on the simple method of measuring microbial populations’ size over time and under different conditions. Many advances have increased the throughput of those assays and enabled the study of non-lab adapted microbes under diverse conditions that widely affect their growth dynamics. Our software provides an all-in-one tool for estimating the growth parameters of microbial cultures and testing for differential growth in a high-throughput and user-friendly fashion without any underlying assumptions about how microbes respond to their growth conditions.

This paper provides a review of recent projects developed through the author’s creative practice and activities across multiple computing and games technologies platforms. These include: a 2D game project made in Unity; an Arduino-based laser puzzle; chiptune breakbeat music made on a Commodore 64; the archival of a collection of Amiga demoscene disks; PETSCII graphics; a controller adapter for the Amiga; and a DJ/VJ performance. While playfully exploring new trajectories, these projects broadly reflect on-going themes present in the author's previous work, such as explorations of the aesthetic paradigms presented by vintage computers, 1990s rave culture, and synaesthesia. The paper will address the various challenges and methodologies used to realise these projects; pedagogical considerations; and the pandemic context in which they have been created and presented.

Este artículo pretende dar a conocer la situación en la que se encontraban las personas que ejercían de amigas, así como las habitaciones donde se dejaban a los niños y niñas pequeños, que recibían el mismo nombre. La mayoría de las amigas no tenían preparación y los espacios donde acogían a los niños estaban en deficientes condiciones., This article aims to publicize the situation in which the people who were friends were found, as well as the rooms where the young children, who received the same name, were left. Most of the friends were unprepared and the spaces where they welcomed the children were in poor condition.

Objective. This study aims to determine the prevalence of risk factors of non-communicable diseases (NCDs) in 16barangays of the AMIGA municipalities of Cavite. Methods. The research is a cross-sectional study. Randomly chosen participants were interviewed using a translatedversion of the WHO Steps questionnaire. Interviewees were then invited to participate in another session wheretheir anthropometric measurements were taken and their fasting blood sugar and cholesterol levels were determined. Results. The research was done in 12 out of the 16 targeted barangays. A total of 1,527 participants were interviewedand 1,123 of them completed the study. The most significant findings in all 12 barangays were a very high rate ofpassive smoking (range of 60-80%); a relatively high proportion of respondents with obesity by all 3 parameters(BMI 29-52%; waist circumference 42-78%; and waist-to-hip ratio 41-78%) despite sufficient intake of fruits andvegetables and more than adequate physical activity; and a high proportion of participants with hypertension (morethan 30% in 8 out of 12 barangays) and diabetes mellitus (more than 8% in 7 out of 12 barangays). Conclusion. A high prevalence of risk factors of NCDs, particularly obesity, hypertension, and diabetes was foundin the 12 barangays of AMIGA that participated in the study. Results of this study should provide the baseline dataagainst which the success of an ongoing program in the area can be measured.

Objectives. This study aims to (1) determine the cardiovascular risk of persons with hypertension and diabetesattending hypertension/diabetic clinics or hypertension/health club meetings in the AMIGA (Alfonso, Mendez,Indang, General Emilio Aguinaldo and Amadeo) municipalities of Cavite; (2) suggest measures to improve thecardiovascular disease (CVD) program in these municipalities using the results of the study. Methods. A cross-sectional study was performed on patients diagnosed with hypertension and/or diabetes whoare attending clinics or club meetings in the barangays of the five AMIGA municipalities of Cavite. Participantswere interviewed using an abbreviated version of the World Health Organization (WHO) STEPS questionnaireon risk factors. The participants’ anthropometric measurements were obtained and their total blood cholesterollevels determined. CVD risk was then estimated using the WHO / International Society of Hypertension (ISH) riskprediction chart for the Western Pacific Region B. Results. 1,032 participants from 27 barangays qualified for the study. Participants were predominantly female(74%); over-all mean age was 58.43 years. Majority of the participants (79.17%) were found to be in the low-riskgroup; 11.34% were in the moderate risk group; 4.46% were in the high-risk group; while 5.05% were in the veryhigh-risk group. Majority of the participants were also found to be obese. Mean total cholesterol was 207.02 mg/dl. Conclusion. Majority of participants were stratified in the low-risk category (

La muongrafía es una técnica de prospección no destructiva que permite la determinación de la estructura interna de grandes estructuras tanto naturales como artificiales, por ejemplo volcanes. Esto es posible al construir una imagen con base en la absorción diferencial del flujo direccional de muones atmosféricos producto de la interacción de rayos cósmicos con la atmósfera. Este trabajo doctoral es desarrollado con el propósito principal de aportar en el avance de la muongrafía como técnica de prospección en Geofísica. El trabajo se compone de dos lineas de trabajo, una experimental y una teórica. La experimental se basa en el desarrollo de un prototipo de detector de astropartículas con base en centelladores plásticos y fotomultiplicadores, para esto se usa una electrónica de adquisición desarrollada para el proyecto AMIGA en el Observatorio Pierre Auger y materiales centelladores de plástico. La segunda linea de trabajo trata del estudio del detector y las estructuras de investigación a través de simulaciones computacionales y modelos teóricos. Durante los dos primeros años se completaron los créditos de cursos solicitados por el doctorado, Ademas se trabajó en el estudio de la respuesta de la electrónica, los pulsos, técnicas de análisis de datos y el acople de fotomultiplicadores con los centelladores. Gracias a esto se avanzo en el desarrollo del prototipo y se investigo la posibilidad de incrementar la resolución espacial a través de la detección sincrónica usando electrónicas conectadas al mismo centellador. Actualmente iniciamos el trabajo en los modelos computacionales, estamos estudiando e investigando con respecto a los candidatos a objetos de estudio, destacando el volcán Copahue, volcán Peteroa y la posibilidad de realizar mediciones bajo tierra.

AMIGA (Auger Muons and Infill for the Ground Array) es una mejora del Observatorio Pierre Auger con el objetivo de complementar el estudio de los rayos cósmicos de ultra alta energía (UHECR) mediante la medición del contenido muónico de las cascadas atmosféricas extensas (EAS). Éste consiste en un arreglo de 61 detectores de agua de efecto Cherenkov ubicado en un espacio más denso en combinación con detectores de centelleo enterrados bajo tierra utilizados para la medición de densidad de muones. Cada detector esta compuesto por tres módulos centelladores, con un área de detección de 10 m2 por módulo, enterrados a 2.3 m de profundidad, resultando un área total de detección de 30 m2. Fotomultiplicadores de silicio (SiPM) miden la cantidad de luz de centelleo generada por las partículas cargadas que atraviesan los módulos. En este trabajo, el diseño de la electrónica del front-end para procesar las señales de esos SiPMs, y los resultados de pruebas realizadas en el laboratorio como también en el sitio del Observatorio Pierre Auger son descriptos. Comparado con el diseño anterior, esta nueva electrónica muestra un mayor rendimiento, una mayor eficiencia y un menor consumo de potencia, e incluye además, un nuevo sistema de adquisición con un rango dinámico ampliado que permite realizar mediciones cercanas al núcleo de la lluvia. El nuevo sistema de adquisición esta basado en la medición de la carga total que la componente muónica de la lluvia cósmica genera en el detector.

Cosmic rays have been studied for more than 100 years, providing valuable information on the measured spectrum and theories to particle propagation and interaction. Potential sources, which could also serve possible acceleration mechanisms, include active galactic nuclei, gamma-ray bursts and supernova shock fronts. Due to our increased understanding of cosmic ray physics and technological improvements on a detector level, measurements have progressed towards even higher energies than before. To understand their origin, it is pertinent to understand their mass composition, energy spectrum and arrival direction. Laboratory-based particle accelerators and low energy cosmic ray experiments have elucidated our understanding of particle interaction, providing insight on possible acceleration and propagation models. However, ultra-high cosmic rays at $10^{20}$ eV are significantly above the highest energies achievable by the LHC (about two orders of magnitude between the center-of-mass energies). They are also very rare; with an incident flux of 1 particle per $km^{2}$ per century at $10^{20}$ eV. Accelerator-based models can be extrapolated to the highest energies. However, it is pertinent for large-scale detectors to be able to measure unique properties of cosmic rays interacting with the detection medium. The Auger is the largest cosmic ray detector to date, covering an area of more than 3000 ${km^{2}}$. It utilizes surface, underground and fluorescence techniques to measure the macroscopic properties of extensive air showers (initiated by a cosmic ray particle interacting with a nucleus in the atmosphere). Through the fluorescence technique the longitudinal profile can be directly observed. From its maximum, $X_{\text{max}}$, the cosmic ray mass can be inferred. However, due to specific operational conditions it has a duty cycle of $\approx15$%, limiting the statistics of more energetic events. The surface and underground detectors can measure data with a duty cycle of $\approx100$%. Most surface detectors are distributed in a triangular grid with a spacing of 1500 m. A small fraction is distributed in an infilled grid with a spacing of 750 m. Furthermore, each surface detector in the filled grid is paired with an underground detector. Their combined information provides another mass composition sensitive parameter -the muon content. Air shower universality capitalizes on the universal shape of the longitudinal profile, irrespective of primary or hadronic model. It encapsulates the underlying shower physics and allows for a reconstruction based on mass-composition sensitive shower parameters (the shower maximum $X_{\text{max}}$, maximum of muon production depth $X^{\mu}_{\text{max}}$ and relative muon content $R_{\mu}$) seen through unique features in the time and signal distributions. The universality approach allows for a highly modular reconstruction algorithm, set as a function of primary energy, mass and geometry. The major focus of this work was the development of the a new signal and time model for secondary particles at ground seen by the WCD and MD, as well as dedicated efforts to effectively process large quantities of simulated air showers. Reconstructed air shower simulations were studied and compared for contemporary high energy hadronic interaction models. In this work, I show how I could successfully model the signal in the detector corresponding to air showers between $10^{17}$ eV and $10^{20}$ eV with uncertainties below the 5% level. The temporal distribution is also successfully modelled, mostly within the 3% level. A novelty, the maximum muon production depth, $X^{\mu}_{\text{max}}$, has been successfully introduced into the MD universality models. With the newly obtained WCD and MD, I could prove that the muon content, $R_{\mu}$, is a global shower variable. Furthermore, first analysis was performed on hybrid reconstructions for the infilled detector setup. Preliminary resolutions of the shower parameters $X_{\text{max}}$ and $X^{\mu}_{\text{max}}$ are of the order 40 ${g cm^{-2}}$ and 50 ${g cm^{-2}}$ respectively, which can be further enhanced. Also, the quality of $R_{\mu}$ has greatly improved, with an uncertainty of only 10%. This work sets an important basis for future analyses (mass composition and shower physics) with data from the WCD and MD. Results obtained in this work could also be used for new detector systems, such as the SSD (part of the AugerPrime upgrade).

The Warhol Museum devoted a small exhibition of select computer graphics from the Andy Warhol collection as well as the Amiga computer on which they were created. The exhibit occupies one room, showcasing Warhol’s computer equipment and some of his artworks. The artifacts include Warhol’s Amiga 1000, on which he created the newly found digital images, and the floppy disks containing them, as well as an Easyl 1000 drawing tablet, and graphics software. Reports on the existence of these early computer graphics created by Warhol and discusses the contents of this exhibition.

The muon densities at 450m from the core for showers above $10^{17.5}$eV and zenith angle between $0^\circ$ and $45^\circ$ are presented. Results are based on 1 year of calibrated data collected by the engineering array of the Auger Muons and Infill for Ground Array (AMIGA) detector. Taking into account systematic uncertainties as well as attenuation effects, the observations suggest that the current hadronic interaction models fail in reproducing the measured number of muons with energies ${>}1$GeV. Simulations at $10^{17.5}$eV and $10^{18.0}$eV show that for EPOS-LHC an increase of 38% is required at both energies, while for QGSJET an increment of 50% and 53% is needed at respective energies. Data have been combined with previous results on muon densities at higher energies showing the match in the evolution of the composition derived with the measurements of depth of the maximum development of the showers in the atmosphere ($X_\text{max}$). The current AMIGA observations show that the variation of the primary masses has no sudden changes in the energy range $10^{17.5}$ to $10^{18.0}$eV.

Using images from Sloan Digital Sky Survey Data Release 8, we have re-examined the morphology of 719 galaxies from the Analysis of the interstellar Medium in Isolated GAlaxies (AMIGA) project, a sample consisting of the most isolated galaxies that have yet been identified. The goal is to further improve the classifications of these galaxies by examining them in the context of the Comprehensive de Vaucouleurs revised Hubble-Sandage (CVRHS) system, which includes recognition of features that go beyond the original de Vaucouleurs point of view. Our results confirm previous findings that isolated galaxies are found across the complete revised Hubble sequence, with intermediate- to late-type (Sb-Sc) spirals being relatively more common. Elmegreen Arm Classifications are also presented, and show that more than 50 per cent of the 514 spirals in the sample for which an arm class (AC) could be judged are grand design (AC 8,9,12). The visual bar fraction for the sample is ≈50 per cent, but only 16 per cent are classified as strongly barred (SB). The dominant family classification is SA (non-barred), the dominant inner variety classification is (s) (pure spiral), and the dominant outer variety classification is no outer ring, pseudo-ring, or lens. The Kolmogorov–Smirnov test is used to check for potential biases in the morphological interpretations, and for any possible relation between rings, bars, and ACs with local environment and far-infrared excess. The connection between morphology and stellar mass is also examined for a subset of the sample. © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society., We acknowledge the support of grant AYA2015-65973-C3-1-R from the European Regional Development Fund (FEDER), through the Spanish Ministry of Economy and Competitveness (MINECO). This work has also been supported by the Spanish Science Ministry 'Centro de Excelencia Severo Ochoa' Program under grant SEV-2017-0709. MJ is supported by a Juan de la Cierva formacion fellowship. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England.

Die Fragen nach dem Ursprung, der Beschleunigung und der Propagation kosmischer Strahlung bei extrem hohen Energien sind noch immer nicht beantwortet. Um verschiedene astrophysikalische Szenarien zu unterscheiden, ist eine präzise Messung der Massenzusammensetzung der kosmischen Strahlung in der Übergangsregion zwischen galaktischer und extragalaktischer kosmischer Strahlung bis zu den höchsten Energien von größter Bedeutung. Die Anzahl von Myonen in ausgedehnten Luftschauern ist eine wichtige Observable um verschiedene Massengruppen der kosmischen Strahlung zu unterscheiden. Aus diesem Grund wird das Pierre-Auger-Observatorium derzeit mit neuen Detektoren erweitert, die es erlauben werden, die myonische Schauerkomponente auf einer Ereignis-zu-Ereignis-Basis zu messen. Als Teil dieses Upgrades wird die AMIGA-Erweiterung, bestehend aus vergrabenen segmentierten Szintillationszählern, direkte Myondichtemessungen ermöglichen. Außerdem wird sie dazu dienen, die indirekten Myonmessungen der Upgradedetektoren zu validieren. Um die Spezifikationen der mittlerweile installierten Upgradedetektoren zu definieren, untersuchen wir den Einfluss des Myonenergiedetektionsschwellwerts auf die Unterscheidbarkeit der Massen von Primärteilchen der kosmischen Strahlung mit detektorunabhängigen Simulationen. Wir stellen fest, dass die Massenunterscheidbarkeit für Detektionsschwellwerte von einigen GeV wächst, obwohl die Anzahl der detektierten Myonen abnimmt. Eine gute Kompositionssensitivität wird jedoch nur für große Detektionsflächen erreicht oder wenn die Tiefe des Schauermaximums zusätzlich aus den Messungen abgeleitet werden kann. Diese Ergebnisse berücksichtigend hat Auger entschieden, Szintillatoren mit einer Fläche von 3.8 m² auf den bereits existierenden Wasser-Cherenkov-Detektoren anzubringen. Um eine auf den Messungen der AMIGA Myonzählern basierende unverzerrte Schätzung der Myondichte zu gewährleisten, optimieren und erweitern wir die bestehende Rekonstruktionsmethode. In diesem Zusammenhang entwickeln wir ein geometrisches Korrekturverfahren für Myonen, die aufgrund ihres schrägen Einfalls ein Signal in mehreren Detektorstreifen hinterlassen. Außerdem schlagen wir eine neue unverzerrte Parametrisierung der lateralen Dichtefunktion der Myonen vor und stellen sicher, dass der optimale Abstand für ihre Auswertung unverändert bleibt. Das Prototyparray für AMIGA, bestehend aus einem Hexagon aus sieben Myondetektoren, ist seit Februar 2015 in Betrieb. Wir wählen die kalibrierten Daten eines Jahres aus und entwickeln eine Methode um Perioden auszuschließen, während derer bestimmte AMIGA-Module nicht funktionsfähig waren, um eine hohe Qualität der Daten zu gewährleisten. Zudem schließen wir fehlerhafte Module aus und korrigieren für die flächenabhängigen Effizienzen der Detektormodule. Weiterhin definieren wir einen zenithwinkelunabhängigen Schätzer ρ₃₅ der Myondichte, indem wir die Abschwächung des Myonsignals durch die Atmosphäre und die Erdschicht oberhalb der vergrabenen Myondetektoren parametrisieren. Die grössten systematischen Unsicherheiten für AMIGA entstehen durch die modulflächenspezifische Effizienzkorrektur, das Setzen des Diskriminatorschwellwerts der einzelnen Szintillatorkanäle, die Dichte des Bodens, die Parametrisierung der lateralen Dichtefunktion der Myonen und die Abschwächungskorrektur. Wir schätzen die einzelnen Beiträge ab und erhalten eine systematische Gesamtunsicherheit von ungefähr 14% von ρ₃₅. Mehrere Experimente haben einen “Myonüberschuss” in ihren Daten beobachtet. Unsere Analyse von AMIGA-Daten bestätigt diesen Unterschied im Myonanteil zwischen Simulationen und Daten bei etwas anderen Energien. Indem wir Xmax-Messungen von Auger als Schätzer der mittleren logarithmischen Masse in Daten verwenden finden wir, dass der Myonanteil in Simulationen um 38% bis 53%, abhängig vom hadronischen Wechselwirkungsmodell, erhöht werden müsste um mit den AMIGA-Ergebnissen übereinzustimmen. Basierend auf den Myondichtemessungen des AMIGA Prototyparrays analysieren wir die Entwicklung der Massenkomposition indem wir die korrigierten Myondichten ρ₃₅ mit einer Potenzgesetzparametrisierung als Funktion der Energie fitten. Zusätzlich berechnen wir die energieabhägige mittlere logarithmische Masse. In Übereinstimmung mit vorherigen Xmax-Messungen des Pierre-Auger-Observatoriums weisen die Ergebnisse auf ein Leichterwerden der Massenkomposition im Energiebereich von 10¹⁷⋅⁴ eV bis ¹⁸⋅³ eV hin. AMIGA wird Ende 2019 vervollständigt sein und bis 2025 Daten nehmen. Obwohl das endgültige Detektordesign im Vergleich zum Prototyparray leicht verändert sein wird, da die Photomultiplier durch Silicon-Photomultiplier ersetzt werden, sind die meisten der in dieser Arbeit entwickelten Verbesserungen der Rekonstruktion anwendbar. Die vorgestellte erste systematische Analyse von Daten des AMIGA Prototyparrays zeigt, dass AMIGA auf dem Weg ist Kompositionsmessungen durchzuführen, die dabei helfen werden astrophysikalische Modelle des Ursprungs und der Propagation ultra-hochenergetischer kosmischer Strahlung einzuschränken.

The Auger Muons and Infill for the Ground Array (AMIGA) aims to both extend the detection range of the Pierre Auger Observatory down to energies $\sim 10^{16.5}~\mathrm{eV}$ and to measure the muon content of extensive air showers. To accomplish these goals, its detection system is composed of an array of coupled water-Cherenkov and scintillation detectors deployed in a graded triangular grid of 433 and 750\,m spacings. At each position, the scintillation detector is buried $2.3~\mathrm{m}$ deep so as to shield it from the air shower electromagnetic component and thus only measure the muon component. These muon detectors have $30~\mathrm{m^2}$ area split into modules, each of them highly segmented in 64 plastic-scintillator strips with an embedded wavelength-shifter optical fiber to transport light to an optical sensor located at the center of the module. During the engineering array phase (finished in November 2017) two module areas ($5~\mathrm{m^2}$ and $10~\mathrm{m^2}$) and two optical sensors (photo-multiplier tubes and silicon-photomultipliers) were tested. In this work, we present the final performance of the muon detectors equipped with silicon-photomultipliers which were thereafter selected as the baseline design for the AMIGA production phase. Analyses and results are based both on laboratory and field measurements., Proceeding of the UHECR 2018 conference, submitted to the forthcoming EPJ Web of Conferences

The Amiga PC architecture was a child of both home video game consoles and PC systems of the early 1980s. The microcomputer revolution of the mid-1970s had given birth to the video game console market and the PC market, which expanded rapidly. In the fall of 1982, Atari alone had total sales of US$2 billion, including video game consoles, game cartridges, and their own PCs [1]. Many companies in the PC market were competing to establish market standards and attract developer support, beginning with S-100 bus machines [2] and the Apple II [3]. IBM entered the PC market with the introduction of the IBM PC in 1981. The Apple Macintosh arrived in 1984, and the Commodore Amiga 1000 computer, the subject of this article, followed in 1985.

Amiga technology came into being decades ago. The concepts (and some of the actual system components) had staying power despite the failure of the original manufacturer. Developers and users around the world continue to push and use Amiga derived and expanded technology. This is more than retrocomputing as a desire to simply reclaim past computing technology. This is an example of continued technology development by a community of invested users, a sort of consumer-led development.

It was observed that the optical crosstalk probability ( C T ) of the silicon photomultipliers (SiPMs) of the electronics in all the AMIGA muon counter modules installed at the Pierre Auger Observatory was reduced by a factor of ∼ 2 . 68 after its deployment. This effect motivated the study of the optical crosstalk in SiPMs, in particular, the external interface optical crosstalk ( E I C T ). In this paper, two laboratory measurements were performed to evaluate the C T , and a model to simulate the E I C T is proposed. We show that combining C T measurements with simulations, the E I C T can be precisely estimated. We also obtained the internal optical crosstalk of the tested SiPM and it was ( 1 . 27 ± 0 . 05 ) % . This study shows that the thickness of the protective window of the SiPM and the optical system to which the SiPM is coupled affects optical crosstalk. We conclude that the E I C T is not negligible and for some cases it is the main contribution to the total optical crosstalk in SiPMs. Taking advantage of the C T variations depending on the optical system to which the SiPM is connected, we propose a method to validate the proper installation of the electronics in the muon counters modules of AMIGA.

Tesis Univ. Granada. Programa Oficial de Posgrado en Física y Matemáticas

Los rayos cósmicos (E > 1014 eV) son conocidos desde hace más de 70 años y, sin embargo, su origen sigue siendo un misterio. Del mismo modo, la posibilidad de una componente fotónica de muy alta energía en el flujo de radiación cósmica es uno de los problemas abiertos en la Física de Astropartículas. La búsqueda de fotones de alta energía complementa las mediciones de los rayos cósmicos y neutrinos hacia una comprensión multi-canal de los fenómenos astrofísicos más energéticos. En particular, el descubrimiento de fotones con energías entre 1016.5 eV y 1018 eV en el flujo de los rayos cósmicos podría ser de particular interés no sólo para el campo de la Física de Astroparticulas, sino también para la Astrofísica y la Física fundamental, ya que son rastreadores de los procesos de mayor energía en el Universo. En la búsqueda de fotones de ultra-alta energía, es crucial definir parámetros sensibles a la composición capaces de rechazar adecuadamente el fondo hadrónico de los rayos cósmicos. El contenido muónico de las lluvias atmosféricas extensas producidas por los rayos cósmicos primarios al entrar en la atmósfera es uno de los aspectos más prometedores que podría conducir a la mejor discriminación posible entre los fotones y los rayos cósmicos hadrónicos. El detector de muones subterráneo AMIGA, como parte de la próxima mejora AugerPrime del Observatorio Pierre Auger, ofrece una oportunidad única y directa para medir muones de alta energía de lluvias atmosféricas extensas, y así, aumentar la sensibilidad del Observatorio a una señal fotónica primaria. La Colaboración Pierre Auger ha propuesto varios parámetros para estudiar una posible componente fotónica de ultra-alta energía en el flujo hadrónico de rayos cósmicos. Sin embargo, su no-observación resultó en límites superiores para energías por encima de 1018 eV. Por otra parte, la ventana energética entre 1016.5 eV y 1018 eV sólo ha sido explorada por los experimentos de KASCADE-Grande y EAS-MSU, que imponen límites superiores al flujo fotónico. Actualmente, este dominio energético no es explorado por el Observatorio Pierre Auger. El objetivo principal de esta tesis es la extensión de la búsqueda de fotones de ultra alta energía hasta ∼ 1016.5 eV. Los estrictos límites superiores teóricos y experimentales al flujo fotónico en estas energías hacen que la búsqueda de una débil señal fotónica en el vasto fondo de los rayos cósmicos hadrónicos sea una tarea desafiante. Por lo tanto, los parámetros sensibles a la señal predominantemente electromagnética de los fotones primarios son de suma importancia. En este marco, definimos y describimos dos nuevos observables sensibles a la composición diseñados para la discriminación fotón/hadrón con el fin de detectar fotones primarios a energías del orden de 1016 eV o mejorar los límites superiores establecidos por experimentos anteriores. El observable Mb combina las densidades de muón medidas por las estaciones de muón subterráneas AMIGA y su distancia al eje de la lluvia, de manera similar al conocido parámetro Sb utilizado anteriormente en las búsquedas fotónicas por la Colaboración Pierre Auger. Por otra parte, el observable Q explota la diferencia en la pendiente de la distribución lateral de partículas entre las lluvias iniciadas por fotones y hadrones. En este último caso, se espera que las lluvias se desarrollen a mayores alturas en la atmósfera y lleguen al suelo con una distribución más plana de partículas. En este trabajo, afinamos ambos observables para ser aplicados en el detector de superficie y detector de muones del Observatorio Auger para energías por encima de Erec = 1016.4 eV y θ < 45°. Un método multiparamétrico, bautizado Mb + Q, es extensamente estudiado y su ejecución se aborda bajo numerosas condiciones. Se demuestra que el rechazo de fondo y la eficiencia de la señal para el método compuesto son adecuados para imponer los mejores límites superiores de todos los experimentos de rayos cósmicos con tan sólo unos pocos años de datos, y en particular mejorarlos por un orden de magnitud al final actualmente planificado de operación de Auger el 31 de diciembre 2025. Considerando la alta exposición del experimento Auger en dirección al centro galáctico, el método descrito en esta tesis representa una herramienta valiosa con un potencial de descubrimiento sin precedentes en la detección de una señal fotónica minúscula en el flujo de rayos cósmicos. Aunque en esta investigación se presenta una estimación ciega de la sensibilidad a un flujo fotónico, está previsto que la aplicación a los datos se lleve a cabo en un futuro próximo para una publicación oficial de la Colaboración Pierre Auger. Cosmic rays (E > 1014 eV) have been known for more than 70 years, and yet their origin remains elusive. Similarly, the possibility of a very-high energy photon component of the cosmic radiation is one of the open problems in Astroparticle Physics. The search for high energy photons complements measurements of cosmic rays and neutrinos towards a multi-messenger understanding of the most energetic astrophysical phenomena. In particular, the discovery of photons with energies between 1016.5 eV and 1018 eV in the cosmic rays flux could be of particular interest not only for the field of Astroparticle Physics, but also for Astrophysics and fundamental Physics, since they are tracers of the highest-energy processes in the Universe. In the search for ultra-high energy photons, it is crucial to define composition-sensitive parameters capable of adequately rejecting the hadronic cosmic-ray background. The muon content of the extensive air showers produced by primary cosmic rays as they enter the atmosphere is one of the most promising aspects that could lead to the best possible discrimination between photons and hadronic cosmic rays. The AMIGA underground muon detector, as a part of the upcoming AugerPrime upgrade for the Pierre Auger Observatory, offers a unique and straight-forward opportunity to directly measure high-energy muons of extensive air showers, and thus, enhance the sensibility of the Observatory to a primary photon signal. The Pierre Auger Collaboration has proposed several parameters in order to study a possible ultra-high energy photon component in the hadronic cosmic-ray flux. However, the nonobservation of photon candidates resulted in upper limits for energies above 1018 eV. On the other hand, the energy window between 1016.5 eV and 1018 eV has only been explored by the KASCADEGrande and the EAS-MSU experiments which impose upper limits to the photon flux. Currently, this energy domain is not explored by the Pierre Auger Observatory. The main objective of this thesis is the extension of the ultra-high energy photon search down to ∼ 1016.5 eV. The stringent theoretical and experimental upper limits to the photon flux at these energies make the search of a weak photon signal in the vast hadronic cosmic-ray background a challenging task. Therefore, parameters sensitive to the predominantly electromagnetic signal from photon primaries are of paramount importance. In this framework, we define and describe two new composition-sensitive observables designed for the photon/hadron discrimination quest in order to either detect photon primaries in the 1016 eV energy domain or improve the upper limits established by previous experiments. The observable Mb combines the muon densities measured by the AMIGA underground muon stations and their distance to the shower axis, similarly to the well-known Sb parameter used previously in photon searches by the Pierre Auger Collaboration. On the other hand, the observable Q exploits the difference in the slope of the lateral distribution of particles between photon- and hadron-initiated showers. In the latter case, the showers are expected to develop higher in the atmosphere and thus they arrive to the ground with a flatter distribution of particles. In this work, we tune both observables to be applied in the surface and muon detector of the Auger Observatory for energies above Erec = 1016.4 eV and θ < 45°. A multiparametric method, baptized Mb+Q, is extensively studied and its performance is addressed under numerous conditions. The background rejection and the signal efficiency for the compound method is proved to be suitable to impose the best upper limits of all the cosmic-ray experiments with only a few years of data, and particularly improve them by one order of magnitude by the end of Auger planned operation at December 31st 2025. Considering the high exposure of the Auger experiment in the direction of the Galactic center, the method described in this thesis represents a valuable tool with an unprecedented discovery potential in the detection of a minuscule photon signal in the cosmic-ray flux. Although a blind estimation of the sensitivity to a photon flux is presented in this research, the application to data is foreseen to be carried out in the near future for a dedicated full-author list paper of the Pierre Auger Collaboration Kosmische Strahlung (E > 1014 eV) ist seit mehr als 70 Jahren bekannt, jedoch bleiben ihren Ursprung unerklärt. Ebenso ist das Vorhandensein einer hochenergetischen Photonenkomponente der kosmischen Strahlung weiterhin eine offene Frage der Astroteilchenphysik. Die Ergänzung von Messungen kosmischer Strahlung und Neutrinos durch hochenergetische Photonen verfeinert unsere Multi-Messenger-Suche von energetischsten astrophysikalischen Phänomenen. Insbesondere die Entdeckung von Photonen mit Energien zwischen 1016.5 eV und 1018 eV im Fluss der kosmischen Strahlung könnte nicht nur für die Astroteilchenphysik relevant sein, sondern auch für die Astrophysik und die Grundlagenphysik, da sie Indikatoren der energiereichsten Prozesse im Universum sind. Bei der Suche nach ultrahochenergetischen Photonen ist es entscheidend, kompositionssensitive Parameter zu definieren, die in der Lage sind, den Untergrund der hadronischen kosmischen Strahlung adäquat zu eliminieren. Der Myonengehalt der Sekundarteilchen ausgedehnter Luftschauer gehört zu den vielversprechendsten Aspekten bei der Unterscheidung zwischen Photonen und hadronischer kosmische Strahlung. AMIGA, ein sich in 2.5 m Bodentiefe befindlicher Myondetektor, ist Teil des AugerPrime-Upgrades für das Pierre-Auger-Observatorium. Es bietet eine einzigartige Lösung, wobei hochenergetische Myonen von ausgedehnten Luftschauern direkt gemessen werden. Damit wird die Sensivilität des Observatoriums zum Nachweis von Photonen als Primärteilchen drastisch verbessert. Es gab bereits mehrere Ansätze der Pierre-Auger-Kollaboration, um eine mögliche ultrahochenergetische Photonenkomponente in der kosmischen Strahlung zu untersuchen. Die Nichtbeobachtung von Photonenkandidaten führte jedoch zu Obergrenzen für Energien über 1018 eV. Andererseits wurde das Energiefenster zwischen 1016.5 eV und 1018 eV nur von der KASCADEGrande und den EAS-MSU-Experimenten untersucht, strikte Obergrenzen des Photonenflusses bestimmten. Derzeit wird dieser Energiebereich im Rahmen des Pierre-Auger-Observatoriums nicht erforscht. Das Hauptziel dieser Arbeit ist die Erweiterung der ultrahochenergetischen Photonensuche bis zu Energien von ∼ 1016.5 eV. Die strengen theoretischen und experimentellen Obergrenzen des Photonenflusses bei diesen Energien macht die Suche nach einem schwachen Photonensignal bei hohem hadronischen Strahlungsuntergrund zu einer herausfordernden Aufgabe. Daher sind Parameter, die auf das überwiegend elektromagnetische Signal empfindlich sind, wie im Falle von Photonen, von äußerster Wichtigkeit. In diesem Rahmen werden zwei neue photonsensitive Parameter definiert und beschrieben, die für die Suche nach der Photonen-/HadronenDiskriminierung entwickelt wurden, um entweder Photonen im Energiebereich 1016 eV zu detektieren oder die Obergrenzen zu verbessern, die durch bisherige Experimente ermittelt wurden. So wie mit dem Sb Parameter, welcher zuvor bei der Photonensuche der Pierre-Auger-Kollaboration verwendet wurde, wird bei Mb die Myondichte der AMIGA-Stationen und deren Abstand zur Schauerachse kombiniert. Die Observable Q nutzt den Unterschied in der Steilheit der lateralen Verteilung der Teilchen zwischen photon- und hadroninduzierten Luftschauern. Im letzteren Fall wird erwartet, dass sich die Luftschauer in der Atmosphäre höher entwickeln und deshalb mit einer flacheren Teilchenverteilung auf den Boden gelangen. In dieser Arbeit werden die Observablen der Oberflächen- und AMIGA-Detektoren so optimiert, dass sie im Energiebereich über Erec = 1016.4 eV und θ < 45° verwendet werden können. Eine multiparametrische Methode, Mb + Q genannt, wird ausführlich untersucht und ihre Leistungfähigkeit wird unter zahlreichen Bedingungen untersucht. Die Untergrundunterdrückung und der Photonnachweis für das multivariate Verfahren sind geeignet zur Bestimmung der striktesten Obergrenzen aller Experimente in diesem Energiebereich innerhalb nur weniger Jahre Messzeit. Bis zum Ende der geplannt Laufzeit des Observatoriums wird eine um eine Größenornung verbesserte Obergrenze erwartet. In Anbetracht der hohen Exposition des AugerExperiments in Richtung des galaktischen Zentrums, stellt die in dieser Arbeit beschriebene Methode ein wertvolles Werkzeug dar eine winziges Photonensignal im galaktischen Strahlungsfluss zu finden. Obwohl im wesentlichen nur eine Blindstudie zur Empfindlichkeit eines Photonenflusses in dieser Studie vorgestellt wird, ist die Anwendung auf Daten in naher Zukunft im Rahmen einer Auger-Publikation in Arbeit. Erst dann dürfen die bisher unbenutzen Daten untersucht werden. Fil: González, Nicolás Martín. Karlsruher Institut für Technologie; Alemania. Consejo Nacional de Investigaciones Científicas y Técnicas. Oficina de Coordinación Administrativa Parque Centenario. Instituto de Tecnología en Detección y Astropartículas. Comisión Nacional de Energía Atómica. Instituto de Tecnología en Detección y Astropartículas. Universidad Nacional de San Martín. Instituto de Tecnología en Detección y Astropartículas; Argentina. Universidad Nacional de San Martín; Argentina

In this thesis, a novel technique is developed to estimate the cosmic-ray mass on a per-event level by combining radio and muon measurements of air showers. The new technique is studied using Monte Carlo simulations of air showers and then verified experimentally based on data from the Muon Detector of AMIGA and the Radio Detector AERA of the Pierre Auger Observatory in Argentina.

The present contribution reports some of the most effective results achieved during the last few years in the frame of three different experiments (GAME, AMIGA, LIFE) of the Italian Institute of Nuclear Physics (INFN). In particular, four different foundry runs have been done using the ALENIA MESFET technology and more than thirty different circuits were designed and tested. Only few of them are reported, with a short description, in the following.

Our view of galaxies has been transformed in recent years with diffuse halo gas surrounding galaxies that contains at least as many metals and baryons as their disks. While single sight lines through galaxy halos seen in absorption have provided key new constraints, they provide only average properties. Our massive neighbor, the Andromeda (M31) galaxy, provides an unique way to study its circumgalactic medium whereby we can study it using not one or two, but ~36 sightlines thanks to its proximity. With our Large HST program — Project AMIGA (Absorption Maps In the Gas of Andromeda), our goals are to determine the spatial distribution of the halo properties of a L* galaxy using 36 background targets at different radii and azimuths. In this brief paper, I discuss briefly the scientific rationale of Project AMIGA and some early science results. In particular, for the first time we have demonstrated that M31 has a gaseous halo that extends to Rvir with as much as metal and baryonic masses than in its disk and has substantial change in its ionization properties with more highly ionized gas found at R ~ Rvir than cooler gas found near the disk.

We conducted a pilot test of a patient navigation intervention (Una Mano Amiga) to address cancer health disparities in three rural counties in southwest New Mexico. We trained two bilingual lay health workers (promotoras) as patient navigators (PNs) to help adult cancer patients and their participating families in Grant, Luna, and Hidalgo counties “navigate” the health care system, including appropriate access to social and financial services. Our hypothesized outcome was a reduction in time from diagnosis to treatment initiation compared to the average time without PNs in each of the three counties (2000–2009). We enrolled 85 eligible patients and 43 eligible family members who had completed psychosocial and demographic forms in this PN intervention. Mean time from cancer diagnosis to treatment initiation among 41 study patients was 59.6 days across the three counties. Mean time from non-intervention comparison data was 47.1 days. In the intervention group, on a 0–10 satisfaction scale (higher = more), patient mean scores for three items ranged from 9.3 to 9.6, family members, 8.9–9.3. Caregiver stress as measured by a Caregiver Self-Assessment score ≥ 10 (highest stress = 16) decreased from 23.8% of caregivers at study entry to 14.3% at follow-up (not statistically significantly different). Although the PN intervention did not decrease time from diagnosis to treatment initiation compared to three comparison counties, positive reactions of patients and family members support further research with larger samples.

The Auger Muon and Infill Ground Array (AMIGA) is a muon detector that is currently being built as part of AugerPrime, the upgrade of the Pierre Auger Observatory. It consists of 30 m$^2$ plastic scintillator counters buried 2.3 m underground and water-Cherenkov detectors at the surface, organized in a periodic 750 m triangular array, and deployed over an area of 23.5 km$^2$. Each counter is composed of three 10 m$^2$ modules segmented into 64 scintillator strips. Two positions of the engineering array were further equipped with "twin" detectors to assess reconstruction uncertainties. AMIGA allows for direct measurement of the muon content of air showers with primary energies above 10$^{17}$ eV. In this work, the detector reconstruction strategy is revisited and the bias induced by particles traversing two adjacent strips, the so-called corner-clipping effect, is thoroughly analyzed. A bias correction based on end-to-end simulations of both the air showers and the detector response is presented. The improved reconstruction method was applied to experimental data acquired by the AMIGA engineering array, and preliminary results of the muon content estimator $\rho_{450}$ (muon density 450 m from the shower axis) are presented.

Resumo Este artigo discute algumas dimensões de minha pesquisa sobre escuta e gestão do sofrimento em serviços de apoio emocional. Focalizei em outro texto as narrativas morais e técnicas de interação como aspectos constitutivos da atuação de tais serviços. Tive como objeto o Centro de Valorização da Vida (CVV), no Rio de Janeiro, e o SOS Voz Amiga, em Lisboa. Aqui procuro dar ênfase às fontes dessas moralidades, procurando investigar os elementos de longa duração que concorreram para que elas se estruturassem. Para isso, dirijo meus interesses especificamente para os atos de fala, buscando proximidades e ressonâncias entre os métodos do CVV e as práticas da confissão e do testemunho. Abstract This article discusses some dimensions of my research on suffering demeanor in emotional support services. I focused in another work on the discourses and interaction techniques as crucial aspects of these services, in particular the Centro de Valorização da Vida (CVV), in Rio de Janeiro, and the SOS Voz Amiga, in Lisbon. Here I try to highlight the sources of these moralities, seeking to investigate the foundational elements that shape their moral arrangements. For this, I am particularly interested in speech acts, exploring proximities and resonances between CVV methods and the practices of confession and testimony.

The Auger Engineering Radio Array (AERA) is a radio detector at the Pierre Auger Observatory and it is dedicated to measure the radio emission of cosmic-ray air showers. AERA is co-located with the underground muon detectors of the Auger Muons and Infill for the Ground Array (AMIGA). This provides a perfect setup to experimentally test the benefits of combining muons and radio emission for estimating the primary mass. We have investigated this combination using air-shower simulations. We compared the performance for mass separation of this new method to alternative methods in which the electrons and muons are measured with particle detectors at the surface. Forshowers with zenith angles below 50° the new method is of comparable performance, and for showers more inclinedthan 50° it is clearly superior. Therefore, measuring the radio signal in addition to the muons significantly improves the mass sensitivity compared to techniques using solely particle measurements.

Computer dealer demos, such as Boing Ball for the Commodore Amiga, were used to impress trade show audiences and retail customers. Dealer demos, such as those used by Commodore International, Atari, and Apple, illustrate how the home computer was socially constructed as a consumer commodity through the interdependent activities of software companies and user communities rather than simply through the marketing strategies of the hardware industry.

El presente artículo se detiene en los modos de elaboración del duelo por la pérdida de una amiga en El desperdicio (2007) de Matilde Sánchez. Partimos de la idea de Derrida acerca de que el discurso funerario se construye sobre la vida y en el cruce entre ficción y verdad. Concebido como una elegía, el relato articula la memoria de la amiga muerta a través de una evocación biográfica, narrada de forma coextensiva e inescindible de la trayectoria política de la Argentina, ya que la narradora parte del presupuesto de que un nombre arrastra una época. Se trata de una memoria que abarca tres décadas de la vida del personaje y que finaliza con su muerte en el 2001, año en que también se produce una debacle político, económica y social en dicho país.O artigo analisa as maneiras em que está construído o luto pela morte de uma amiga no El desperdício (2007) de Matilde Sánchez. Partimos da ideia de Derrida em torno do discurso funerário como um discurso organizado em torno da vida e do entrecruzamento entre a ficção e a verdade. Concebido como uma elegia, o relato elabora a memória da amiga morta através de uma evocação biográfica, narrada de forma coextensiva e inseparável da trajetória política da Argentina, já que a narradora parte da ideia de que um nome próprio carrega consigo uma época. Trata-se de uma memória que abrange três décadas da vida da personagem, finalizando com a sua morte no ano 2001, no qual também se produz uma débâcle política, econômica e social nesse país.This paper focuses on the ways of construction of grief due to someone's loss of a female friend in El desperdicio (2007) by Matilde Sánchez. Our starting point is Derrida's idea that funerary discourse deals with life and is built at the crossroads between fact and fiction. Composed as an elegy, the account creates the memory of the dead friend through a biographic evocation. It moves forward as Argentina's polítical course does and it is narrated as an integral part of it, since the narrator assumes that a name goes along with an age.This memory spans three decades of the character's life and ends with her death in 2001. In that same year, political, economic and social collapse devastated the country.

Muons from extensive air shower with energy greater than or equivalent to 1 GeV propagating in the soil are able to reach the AMIGA (Auger Muons and Infill for the Ground Array) detector. Although the air shower muonic component is attenuated much less than the electromagnetic component, the shielding of approximately 2.25 m of soil adds 540 g/cm2 of vertical mass. Thus, in order to better understand attenuation mechanisms (shielding effects) of muons, a Monte Carlo simulation with Geant4 was made to determine the muon energy threshold. This threshold can be used to test the Geant4 simulation program, since the muon energy threshold is well calculated via the Bethe-Bloch formula. From the energy thresholds and the energy distribution at ground level for different particles from extensive air showers, the contribution of those particles to the data recorded by the detectors can be calculated. This contribution is crucial to correctly determine the number of muons in an extensive air shower, which is one of the main aims of the AMIGA enhancement.

Despite the significant experimental effort made in the last decades, the origin of the ultra high energy cosmic rays is still unknown. The chemical composition of these energetic particles car- ries key astrophysical information to identify where they come from. It is well known that the muon content of the showers generated by the interaction of the cosmic rays with air molecules, is very sensitive to the primary particle type. Therefore, the measurement of the number of muons at ground level is an essential tool to infer the cosmic ray mass composition. We introduce a novel method to reconstruct the lateral distribution of muons with an array of counters buried under- ground like AMIGA, one of the Pierre Auger Observatory detector systems. The reconstruction builds on a previous method we recently presented by considering the detector time resolution. With the new method more events can be reconstructed than with the previous one. In addition the statistical uncertainty of the measured number of muons is reduced, allowing for a better primary mass discrimination.