Total eclipse of the heart: the AM CVn Gaia14aae/ASSASN-14cn

We report the discovery and characterization of a deeply eclipsing AM CVn-system, Gaia14aae (=ASSASN-14cn). Gaia14aae was identified independently by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al.) and by the Gaia Science Alerts project, during two separate outbursts. A third outburst is seen in archival Pan-STARRS-1 (PS1; Schlafly et al.; Tonry et al.; Magnier et al.) and ASAS-SN data. Spectroscopy reveals a hot, hydrogen-deficient spectrum with clear double-peaked emission lines, consistent with an accreting double-degenerate classification. We use follow-up photometry to constrain the orbital parameters of the system. We find an orbital period of 49.71 min, which places Gaia14aae at the long period extremum of the outbursting AM CVn period distribution. Gaia14aae is dominated by the light from its accreting white dwarf (WD). Assuming an orbital inclination of 90° for the binary system, the contact phases of the WD lead to lower limits of 0.78 and 0.015 M⊙ on the masses of the accretor and donor, respectively, and a lower limit on the mass ratio of 0.019. Gaia14aae is only the third eclipsing AM CVn star known, and the first in which the WD is totally eclipsed. Using a helium WD model, we estimate the accretor's effective temperature to be 12 900 ± 200 K. The three outburst events occurred within four months of each other, while no other outburst activity is seen in the previous 8 yr of Catalina Real-time Transient Survey (CRTS; Drake et al.), Pan-STARRS-1 and ASAS-SN data. This suggests that these events might be rebrightenings of the first outburst rather than individual events.

A Correlation Between Host Star Activity and Planet Mass for Close-in Extrasolar Planets?

The activity levels of stars are influenced by several stellar properties, such as stellar rotation, spectral type, and the presence of stellar companions. Analogous to binaries, planetary companions are also thought to be able to cause higher activity levels in their host stars, although at lower levels. Especially in X-rays, such influences are hard to detect because coronae of cool stars exhibit a considerable amount of intrinsic variability. Recently, a correlation between the mass of close-in exoplanets and their host star's X-ray luminosity has been detected, based on archival X-ray data from the ROSAT All-Sky Survey. This finding has been interpreted as evidence for star-planet interactions. We show in our analysis that this correlation is caused by selection effects due to the flux limit of the X-ray data used and due to the intrinsic planet detectability of the radial velocity method, and thus does not trace possible planet-induced effects. We also show that the correlation is not present in a corresponding complete sample derived from combined XMM-Newton and ROSAT data.

Introducing the CTA concept

The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project. © 2013 Elsevier B.V. All rights reserved.

The Rossiter-McLaughlin effect reloaded: Probing the 3D spin-orbit geometry, differential stellar rotation, and the spatially-resolved stellar spectrum of star-planet systems

When a planet transits its host star, it blocks regions of the stellar surface from view; this causes a distortion of the spectral lines and a change in the line-of-sight (LOS) velocities, known as the Rossiter-McLaughlin (RM) effect. Since the LOS velocities depend, in part, on the stellar rotation, the RM waveform is sensitive to the star-planet alignment (which provides information on the system’s dynamical history). We present a new RM modelling technique that directly measures the spatially-resolved stellar spectrum behind the planet. This is done by scaling the continuum flux of the (HARPS) spectra by the transit light curve, and then subtracting the infrom the out-of-transit spectra to isolate the starlight behind the planet. This technique does not assume any shape for the intrinsic local profiles. In it, we also allow for differential stellar rotation and centre-to-limb variations in the convective blueshift. We apply this technique to HD 189733 and compare to 3D magnetohydrodynamic (MHD) simulations. We reject rigid body rotation with high confidence (>99% probability), which allows us to determine the occulted stellar latitudes and measure the stellar inclination. In turn, we determine both the sky-projected (λ ≈ −0.4 ± 0.2◦) and true 3D obliquity (ψ ≈ 7+12 −4 ◦ ). We also find good agreement with the MHD simulations, with no significant centre-to-limb variations detectable in the local profiles. Hence, this technique provides a new powerful tool that can probe stellar photospheres, differential rotation, determine 3D obliquities, and remove sky-projection biases in planet migration theories. This technique can be implemented with existing instrumentation, but will become even more powerful with the next generation of high-precision radial velocity spectrographs.

A criança pinta o céu de “verde”. Até que ponto lhe devemos dizer que o céu é azul?

Relatório de estágio apresentado para a obtenção do grau de Mestre em Ensino pré-escolar e 1º ciclo do ensino básico

Local object gist: meaningful shapes and spatial layout at a very early stage of visual processing

In his introduction, Pinna (2010) quoted one of Wertheimer’s observations: “I stand at the window and see a house, trees, sky. Theoretically I might say there were 327 brightnesses and nuances of color. Do I have ‘327’? No. I have sky, house, and trees.” This seems quite remarkable, for Max Wertheimer, together with Kurt Koffka and Wolfgang Koehler, was a pioneer of Gestalt Theory: perceptual organisation was tackled considering grouping rules of line and edge elements in relation to figure-ground segregation, i.e., a meaningful object (the figure) as perceived against a complex background (the ground). At the lowest level – line and edge elements – Wertheimer (1923) himself formulated grouping principles on the basis of proximity, good continuation, convexity, symmetry and, often forgotten, past experience of the observer. Rubin (1921) formulated rules for figure-ground segregation using surroundedness, size and orientation, but also convexity and symmetry. Almost a century of research into Gestalt later, Pinna and Reeves (2006) introduced the notion of figurality, meant to represent the integrated set of properties of visual objects, from the principles of grouping and figure-ground to the colour and volume of objects with shading. Pinna, in 2010, went one important step further and studied perceptual meaning, i.e., the interpretation of complex figures on the basis of past experience of the observer. Re-establishing a link to Wertheimer’s rule about past experience, he formulated five propositions, three definitions and seven properties on the basis of observations made on graphically manipulated patterns. For example, he introduced the illusion of meaning by comics-like elements suggesting wind, therefore inducing a learned interpretation. His last figure shows a regular array of squares but with irregular positions on the right side. This pile of (ir)regular squares can be interpreted as the result of an earthquake which destroyed part of an apartment block. This is much more intuitive, direct and economic than describing the complexity of the array of squares.

Dimensions of Mediterranean Diet: world cultural heritage

The book "Dimensions of Mediterranean diet" develops the reflection around the Mediterranean Diet concept - Intangible Cultural Heritage, which took place by initiative of the University of Algarve, during the first cycle of Seminars on Mediterranean Diet, in 2013. Starting with the multiplicity of this concept, the authors follow exploring the reality of this way of life (between the sky and the earth), which is the result of an age-old training process, integrates a habit of eating well in a healthy life practice and is a vehicle for future sustainability. The images accompanying the text portray this Mediterranean identity, straight from Algarve current realities.

The relation between content providers and distributors: Lessons from the regulation of television distribution in the United Kingdom

Using the United Kingdom (UK) as a case study, this article analyses the growing commercial and regulatory significance of broadcaster-distributor relations within the contemporary television industry. The first part of the article argues that despite important changes in broadcast delivery technology, more recently shaped by the growth of the Internet, and the associated growth of options of receiving television content, the traditional delivery platforms (digital terrestrial, satellite and cable) remain by far the preferred choice for viewers in Britain. At the same time, public service broadcasters continue to be the biggest investors in domestic original non-sport content and account for over half of all television viewing. The strength of PSBs in content and their growing reliance on commercial proprietary subscription platforms (cable and satellite) and gradually on the Internet presents challenges in the nexus between broadcasters and distributors. The article focuses on the debate over retransmission fees between PSBs and Sky, and on the question of whether Sky should be required to offer some of its premium content to rival pay-TV platforms. These two examples highlight the impact regulatory intervention can have on the balance of power between broadcasters and distributors. The article concludes that such debates concerning the commercial relations between content providers and distributors will remain pivotal and become more heated given that similar issues are raised in the Internet environment.

Acquisition and transfer of experiential learning from rock climbing to the corporate workplace

There were three purposes to this study. The first purpose was to determine how learning can be influenced by various factors i~ the rock climbing experience. The second purpose was to examine what people can learn from the rock climbing experience. The third purpose was to investigate whether that learning can transfer from the rock climbing experience to the subjects' real life in the workplace. Ninety employees from a financial corporation in the Niagara Region volunteered for this study. All subjects were surveyed throughout a one-day treatment. Ten were purposefully selected one month later for interviews. Ten themes emerged from the subjects in terms of what was learned. Inspiration, motivation, and determination, preparation, goals and limitations, perceptions and expectations, confidence and risk taking, trust and support, teamwork, feedback and encouragement, learning from failure, and finally, skills and flow. All participants were able to transfer what was learned back to the workplace. The results of this study suggested that subjects' learning was influenced by their ability to: take risks in a safe environment, fail without penalty, support each other, plan without time constraints, and enjoy the company of fellow workers that they wouldn't normally associate with. Future directions for research should include different types of treatments such as white water rafting, sky diving, tall ship sailing, or caving.

Airplane Invoice, 1949

An invoice for a Luscombe Silvaire, Model 8-A Sky Pal plane with additional items installed. The total for the invoice is $2541.63 for all items. The invoice was made out by Aero Activities Limited, Barker Airport, Toronto 10, Ontario. There is a handwritten note at the top of the invoice that reads, "Our 1st airplane".

Maid of the Mist, Niagara, U.S.A.

The description of the image is "(6) Majestically Grand - the Falls from the 'Maid of the Mist,' Niagara, U.S.A.". The reverse of the image reads "You are on the deck of the small but sturdy little steamer that runs along near the foot of the falls. At this moment you are pretty nearly mid-stream, looking south. The American shore are up over your left shoulder. That tall, dark cliff at the extreme left of what you see is Goat Island. The people up there outlined against the sky look like dolls and no wonder; they are more than 160 feet above your head. Some of them are looking off over the unspeakable grandeurs of the Horseshoe Fall there at the right; some are without doubt looking down at the very boat and remarking that the passengers look like dolls. It is an awesome experience to go so near that never-ceasing downpour of waters from the sky. The air is full of the roar and iridescent spray, and it seems as if the boat must be drawn in under the overwhelming floods never to rise again. Yet, curiously enough, the river right around the boat is not so madly excited as you might expect. It seems more like some great creature, dazed, bewildered, stunned by some incredible experience and not yet quite aware of what has happened. (When it gets down into the Whirlpool Rapids, two miles below here, it is dramatically alive to its situation!) The gigantic curve of the cliffs, reaching in up-stream straight ahead, makes a contour line of over 3000 feet before it comes up against the Canadian banks on the west (right). Geologists say that the Falls ages ago must have been at least seven miles farther down the river (behind you) and have gradually won their way back. Even now the curve of the Horseshoe is worn away from two to four feet in a year. No wonder; 12, 000, 000 cubic feet of water (about 375, 000 tons) sweep over the rocks in one minute, and the same the next minute and the next and the next. See Niagara through the Stereoscope, with special maps locating all the landmarks about the Falls.

Recherche d’étoiles jeunes de faible masse dans le voisinage solaire

Formées lors de l’effondrement gravitationnel d’un nuage de gaz moléculaire, les étoiles naissantes auront différentes masses variant entre 0.08 et environ 100M . La majorité de la population stellaire de la Galaxie est constituée d’étoiles dont la masse est inférieure à environ 0.6 M . Le dernier évènement de formation stellaire dans le voisinage solaire s’est produit dans la bulle locale il y a au plus 100 millions d’années, vraisemblablement provoqué par le passage d’une onde de choc dans le bras local de la Galaxie. C’est ainsi que se formèrent de jeunes associations d’étoiles dont les membres se caractérisent en particulier par une vitesse spatiale et une position commune dans la Galaxie. Les associations jeunes étant peu densément peuplées et relativement proches du Soleil, leurs membres se font plutôt rares et dispersés sur toute la voûte céleste. Jusqu’à présent, surtout les étoiles les plus massives (brillantes) ont été répertoriées. Les étoiles jeunes de faible masse, constituant la majorité de la population, restent pour la plupart à être identifiées. Les étoiles jeunes de faible masse représentent une population clef pour contraindre les modèles évolutifs des étoiles M et des naines brunes. Elles sont également d’excellentes candidates pour chercher des exoplanètes via les techniques d’imagerie directe. Ce mémoire présente une nouvelle méthode utilisant un modèle cinématique enrichi d’une analyse statistique Bayesienne pour identifier des étoiles jeunes de faible masse dans les associations beta Pictoris, Tucana-Horologium et AB Doradus. À partir d’un échantillon de 1080 étoiles K et M, toutes comportant des indicateurs de jeunesse tels l’émission Halpha et une forte luminosité dans les rayons X, leurs propriétés cinématiques (mouvement propre) et photométriques sont analysées pour en extraire 98 candidates hautement probables membres d’une des trois associations. Une confirmation de leur statut comme membre nécessitera en particulier une mesure de leur vitesse radiale (prédit par notre analyse) et une mesure de la largeur équivalente du lithium à 6708 Å pour mieux contraindre leur âge.

Effets de l'atmosphère terrestre sur les spectres de naines brunes

Les naines brunes sont des astres incapables de déclencher et soutenir des réactions nucléaires dans leur cœur. En l’absence de cette source d’énergie, leur luminosité diminue avec le temps jusqu’à leur extinction complète. Leur flux aux longueurs d’onde de 0,8 à 2,35 μm est particulièrement altéré par l’humidité contenue dans l’atmosphère terrestre, ce qui complique l’étude de ces astres. Le but de la présente recherche est de vérifier si la division par un spectre d’étoile A0 est un moyen de corriger l’altération causée par l’atmosphère terrestre sur cette partie de leur spectre. Tout d’abord, des notions, pertinentes à la compréhension de ce travail, sont abordées. L’introduction présente quelques notions sur les naines brunes et sur l’atmosphère terrestre. Le deuxième chapitre concerne le traitement des données. Il traite de la calibration, de la mise en évidence du problème de non-répétabilité de la position de la fente du spectromètre SIMON ainsi que de ses causes. Il porte aussi sur l’uniformisation de la réponse des pixels et de la soustraction du ciel pour extraire les spectres. La méthode employée pour étudier l’effet de l’atmosphère terrestre sur les spectres de naines brunes y est présentée. Le troisième chapitre analyse les résultats obtenus par l’utilisation de l’étoile de référence de type A0 comme calibration pour corriger le spectre de naine brune, en assumant un même effet de l’atmosphère terrestre sur les deux types d’astres. Nous ne pouvons conclure, avec certitude, que l’absorption tellurique affecte de la même façon les deux spectres ni de quelle façon exactement ils sont affectés. Une recherche supplémentaire nécessitant de nouvelles prises de données à des masses d’air et à des taux d’humidité variés est requise.

Détection de nouvelles candidates au rang de naines brunes de types spectraux plus tardifs que T5 avec le Wide-field Infrared Survey Explorer (WISE)

Les naines brunes sont, en termes de masse, les objets astrophysiques intermédiaires entre les planètes géantes gazeuses et les étoiles de faible masse. Elles se forment de la même manière que les étoiles, par contraction gravitationnelle d’un fragment de nuage de gaz moléculaire ayant atteint la limite de Jeans, mais se différencient par leur incapa- cité à produire les réactions de fusion de l’hydrogène dans leur cœur. Les naines brunes sont par conséquent des objets qui se refroidissent graduellement, et dont les propriétés spectrales évoluent au cours du temps. Ce mémoire présente la recherche de nouvelles candidates de type spectral T tardif et Y, dans le but de compléter le relevé des naines brunes du voisinage solaire. Cette recherche est motivée par deux objectifs principaux. Premièrement, un échantillon com- plet des objets de faible masse est nécessaire pour contraindre correctement la limite aux faibles masses de la fonction de masse initiale des nuages interstellaires, problème clé en astrophysique actuellement. Deuxièmement, les naines brunes de types spectraux tardifs sont les objets stellaires dont les propriétés atmosphériques sont les plus semblables à celles des planètes géantes gazeuses. Par conséquent, la recherche de nouvelles naines brunes permet indirectement d’améliorer nos connaissances des exoplanètes, sans être contraints par la proximité d’étoiles brillantes. À partir du WISE All-Sky Source Catalog, nous avons établi un échantillon de 55 candidates naines brunes répondant aux critères photométriques attendus. Parmi ces can- didates, 17 ont fait l’objet d’un suivi photométrique en bande J à l’Observatoire du Mont-Mégantic, et 9 ont pu être détectées. De ces 9 détections, 4 objets présentent des mouvements propres cohérents avec ceux de naines brunes.

Étude comparative des paramètres atmosphériques d'étoiles naines blanches déterminés par les techniques photométrique et spectroscopique

Ce mémoire présente une analyse comparative des paramètres atmosphériques obtenus à l’aide des techniques photométrique et spectroscopique. Pour y parvenir, les données photométriques et spectroscopiques de 1375 naines blanches de type DA tirées du Sloan Digital Sky Survey (SDSS) ainsi que les données spectroscopiques du Villanova White Dwarf Catalog ont été utilisées. Il a d’abord fallu s’assurer que les données photométriques et spectroscopiques étaient bien calibrées. L’analyse photométrique a démontré que la photométrie ugriz ne semblait pas avoir de problème de calibration autre que le décalage des points zéro, qui est compensé en appliquant les corrections photométriques appropriées. De plus, le fait que le filtre u laisse passer le flux à certaines longueurs d’onde dans le rouge ne semble pas affecter la détermination des paramètres atmosphériques. L’analyse spectroscopique a ensuite confirmé que l’application de fonctions de correction permettant de tenir compte des effets hydrodynamiques 3D est la solution au problème de log g élevés. La comparaison des informations tirées des données spectroscopiques des deux différentes sources suggère que la calibration des spectres du SDSS n’est toujours pas au point. Les paramètres atmosphériques déterminés à l’aide des deux techniques ont ensuite été comparés et les températures photométriques sont systématiquement plus faibles que celles obtenues à partir des données spectroscopiques. Cet effet systématique pourrait être causé par les profils de raies utilisés dans les modèles d’atmosphère. Une méthode permettant d’obtenir une estimation de la gravité de surface d’une naine blanche à partir de sa photométrie a aussi été développée.