Structure from Stereo and Motion

Stereopsis and motion parallax are two methods for recovering three dimensional shape. Theoretical analyses of each method show that neither alone can recover rigid 3D shapes correctly unless other information, such as perspective, is included. The solutions for recovering rigid structure from motion have a reflection ambiguity; the depth scale of the stereoscopic solution will not be known unless the fixation distance is specified in units of interpupil separation. (Hence the configuration will appear distorted.) However, the correct configuration and the disposition of a rigid 3D shape can be recovered if stereopsis and motion are integrated, for then a unique solution follows from a set of linear equations. The correct interpretation requires only three points and two stereo views.

The Anxiety of the Image

Kear, A. (2005). The Anxiety of the Image. Parallax, 11 (3), 107-116. RAE2008

Chemically tagging the Hyades stream: does it partly originate from the Hyades cluster?

The Hyades stream has long been thought to be a dispersed vestige of the Hyades cluster. However, recent analyses of the parallax distribution, of the mass function, and of the action-space distribution of stream stars have shown it to be rather composed of orbits trapped at a resonance of a density disturbance. This resonant scenario should leave a clearly different signature in the element abundances of stream stars than the dispersed cluster scenario, since the Hyades cluster is chemically homogeneous. Here, we study the metallicity as well as the element abundances of Li, Na, Mg, Fe, Zr, Ba, La, Ce, Nd and Eu for a random sample of stars belonging to the Hyades stream, and compare them with those of stars from the Hyades cluster. From this analysis: (i) we independently confirm that the Hyades stream cannot be solely composed of stars originating in the Hyades cluster; (ii) we show thatsomestars (namely 2/21) from the Hyades stream nevertheless have abundances compatible with an origin in the cluster; (iii) we emphasize that the use of Li as a chemical tag of the cluster origin of main-sequence stars is very efficient in the range 5500K ≤Teff≤ 6200K, since the Li sequence in the Hyades cluster is very tight, while at the same time spanning a large abundance range; (iv) we show that, while this evaporated population has a metallicity excess of ~0.2 dex with respect to the local thin-disc population, identical to that of the Hyades cluster, the remainder of the Hyades stream population has still a metallicity excess of ~0.06-0.15 dex, consistent with an origin in the inner Galaxy and (v) we show that the Hyades stream can be interpreted as an inner 4:1 resonance of the spiral pattern: this then also reproduces an orbital family compatible with the Sirius stream, and places the origin of the Hyades stream up to 1kpc inwards from the solar radius, which might explain the observed metallicity excess of the stream population. © 2011 The Authors Monthly Notices of the Royal Astronomical Society © 2011 RAS.

Early-type stars observed in the ESO UVES Paranal Observatory Project - III. Sub-parsec and AU-scale structure in the interstellar medium

UVES interstellar observations from the Paranal Observatory Project are presented for early-type stars located in the line of sight to the nearby open clusters IC 2391 (Omni Vel) and NGC 6475 (M7), with spectroscopic resolution R similar to 80 000 and signal-to-noise ratios in the Ti II (3383 angstrom), Ca II K, CH+ (4232 angstrom), Na I D and K I (7698 angstrom) lines of several hundred. The sightlines are a mixture of cluster and non-cluster objects. A total of 22 early-type stars (A and B type) are present in our sample towards IC 2391, with 21 towards NGC 6475/M7, and enable us to probe for differences in column density on scales from similar to 0.07 to 7.3 and similar to 0.05 to 4.9 pc in the respective clusters. Additionally, towards Praesepe the Na I D interstellar variation only is probed towards 13 sightlines and transverse scales of similar to 0.16-10.7 pc at R = 70 000. Towards IC 2391 variations are found in Ti II, Ca II K and Na I D column density in different sightlines of up to 0.7, 1.0 and 1.8 dex (excluding one star), respectively. This kind of variability correlates well with the Hipparcos parallax of the objects, and probes structure within the Local Bubble. For cluster-only objects the variations are 0.3, 0.3 and 0.5 dex, respectively. For the field of view towards NGC6475 the corresponding maximum variations are somewhat smaller, being 0.5, 0.3, 0.8 and 1.0 dex for Ti II, Ca II K, Na I and K I, respectively, for all objects and 0.4, 0.2, 0.6 and 0.7 dex for the cluster-only objects. These are uncorrelated with parallax, and again demonstrate that Ca II K tends to be more smoothly distributed than Na I D. A few likely cluster sightlines show evidence for CH+ and variations in this molecular species of a factor of 10 in equivalent width over sub-pc scales. Towards Praesepe variation in interstellar Na I D is small, being a maximum of only similar to 0.4 dex (including measurement errors), but with fewer sightlines studied. Overall, the scatter in the data is similar for the singly ionized species Ti II and Ca II, lending more support to the hypothesis that these two species sample similar parts of the interstellar medium (ISM). This also appears to be the case for the neutral species Na I D and K I in the one cluster studied. Finally, multiple-epoch observations from a variety of archive sources are used to search for astronomical unit (au) scale structure in the ISM towards 46 sightlines. There are tentative indications of structure on scales of tens to thousands of au for three sightlines. Future observations will confirm the veracity or otherwise of the time-variable components and others presented.

The anomaly in the candidate microlensing event PA-99-N2

The light curve of PA-99-N2, one of the recently announced microlensing candidates toward M31, shows small deviations from the standard Paczynski form. We explore a number of possible explanations, including correlations with the seeing, the parallax effect, and a binary lens. We find that the observations are consistent with an unresolved red giant branch or asymptotic giant branch star in M31 being microlensed by a binary lens. We find that the best-fit binary lens mass ratio is similar to1.2x10(-2), which is one of the most extreme values found for a binary lens so far. If both the source and lens lie in the M31 disk, then the standard M31 model predicts the probable mass range of the system to be 0.02-3.6 M-circle dot (95% confidence limit). In this scenario, the mass of the secondary component is therefore likely to be below the hydrogen-burning limit. On the other hand, if a compact halo object in M31 is lensing a disk or spheroid source, then the total lens mass is likely to lie between 0.09 and 32 M-circle dot, which is consistent with the primary being a stellar remnant and the secondary being a low-mass star or brown dwarf. The optical depth (or, alternatively, the differential rate) along the line of sight toward the event indicates that a halo lens is more likely than a stellar lens, provided that dark compact objects comprise no less than 15% (or 5%) of halos.

Characterizing K2 Planet Discoveries: A super-Earth transiting the bright K-dwarf HIP 116454

We report the first planet discovery from the two-wheeled Kepler (K2) mission: HIP 116454 b. The host star HIP 116454 is a bright (V = 10.1, K = 8.0) K1 dwarf with high proper motion and a parallax-based distance of 55.2 +/- 5.4 pc. Based on high-resolution optical spectroscopy, we find that the host star is metal-poor with [Fe/H]= -0.16 +/- 0.08 and has a radius R-star = 0.716 +/- 0.024 R-circle dot and mass M-star = 0.775 +/- 0.027M(circle dot). The star was observed by the Kepler spacecraft during its Two-Wheeled Concept Engineering Test in 2014 February. During the 9 days of observations, K2 observed a single transit event. Using a new K2 photometric analysis technique, we are able to correct small telescope drifts and recover the observed transit at high confidence, corresponding to a planetary radius of R-p = 2.53 +/- 0.18 R-circle plus. Radial velocity observations with the HARPS-N spectrograph reveal a 11.82 +/- 1.33 M-circle plus planet in a 9.1 day orbit, consistent with the transit depth, duration, and ephemeris. Follow-up photometric measurements from the MOST satellite confirm the transit observed in the K2 photometry and provide a refined ephemeris, making HIP 116454 b amenable for future follow-up observations of this latest addition to the growing population of transiting super-Earths around nearby, bright stars.

Dublin 1916: theatre of revolt

In his essay, Anti-Object, Kengo Kuma proposes that architecture cannot and should not be understood as object alone but instead always as series of networks and connections, relationships within space and through form. Some of these relationships are tangible, others are invisible. Stan Allen and James Corner have also called for an architecture that is more performative and operative – ‘less concerned with what buildings look like and more concerned with what they do’ – as means of effecting a more intimate and promiscuous relationship between infrastructure, urbanism and buildings. According to Allen this expanding filed offers a reclamation of some of the areas ceded by architecture following disciplinary specialization:

‘Territory, communication and speed are properly infrastructural problems and architecture as a discipline has developed specific technical means to deal with these variables. Mapping, projection, calculation, notation and visualization are among architecture’s traditional tools for operating at the very large scale’.

The motorway may not look like it – partly because we are no longer accustomed to think about it as such – but it is a site for and of architecture, a territory where architecture can be critical and active. If the limits of the discipline have narrowed, then one of the functions of a school of architecture must be an attempt occupy those areas of the built environment where architecture is no longer, or has yet to reach. If this is a project about reclamation of a landscape, it is also a challenge to some of the boundaries that surround architecture and often confine it, as Kuma suggests, to the appreciation of isolated objects.

M:NI 2014-15
We tend to think of the motorway as a thing or an object, something that has a singular function. Historically this is how it has been seen, with engineers designing bridges and embankments and suchlike with zeal … These objects like the M3 Urban Motorway, Belfast’s own Westway, are beautiful of course, but they have caused considerable damage to the city they were inflicted upon.

Actually, it’s the fact that we have seen the motorway as a solid object that has caused this problem. The motorway actually is a fluid and dynamic thing, and it should be seen as such: in fact it’s not an organ at all but actually tissue – something that connects rather than is. Once we start to see the motorway as tissue, it opens up new propositions about what the motorway is, is used for and does. This new dynamic and connective view unlocks the stasis of the motorway as edifice, and allows adaptation to happen: adaptation to old contexts that were ignored by the planners, and adaptation to new contexts that have arisen because of or in spite of our best efforts.

Motorways as tissue are more than just infrastructures: they are landscapes. These landscapes can be seen as surfaces on which flows take place, not only of cars, buses and lorries, but also of the globalized goods carried and the lifestyles and mobilities enabled. Here the infinite speed of urban change of thought transcends the declared speed limit [70 mph] of the motorway, in that a consignment of bananas can cause soil erosion in Equador, or the delivery of a new iphone can unlock connections and ideas the world over.

So what is this new landscape to be like? It may be a parallax-shifting, cognitive looking glass; a drone scape of energy transformation; a collective farm, or maybe part of a hospital. But what’s for sure, is that it is never fixed nor static: it pulses like a heartbeat through that most bland of landscapes, the countryside. It transmits forces like a Caribbean hurricane creating surf on an Atlantic Storm Beach: alien forces that mutate and re-form these places screaming into new, unclear and unintended futures.

And this future is clear: the future is urban. In this small rural country, motorways as tissue have made the whole of it: countryside, mountain, sea and town, into one singular, homogenous and hyper-connected, generic city.

Goodbye, place. Hello, surface!

MNI: Motorway Notation Network

In his essay, Anti-Object, Kengo Kuma proposes that architecture cannot and should not be understood as object alone but instead always as series of networks and connections, relationships within space and through form. Some of these relationships are tangible, others are invisible. Stan Allen and James Corner have also called for an architecture that is more performative and operative – ‘less concerned with what buildings look like and more concerned with what they do’ – as means of effecting a more intimate and promiscuous relationship between infrastructure, urbanism and buildings. According to Allen this expanding filed offers a reclamation of some of the areas ceded by architecture following disciplinary specialization:

‘Territory, communication and speed are properly infrastructural problems and architecture as a discipline has developed specific technical means to deal with these variables. Mapping, projection, calculation, notation and visualization are among architecture’s traditional tools for operating at the very large scale’.

The motorway may not look like it – partly because we are no longer accustomed to think about it as such – but it is a site for and of architecture, a territory where architecture can be critical and active. If the limits of the discipline have narrowed, then one of the functions of a school of architecture must be an attempt occupy those areas of the built environment where architecture is no longer, or has yet to reach. If this is a project about reclamation of a landscape, it is also a challenge to some of the boundaries that surround architecture and often confine it, as Kuma suggests, to the appreciation of isolated objects.

M:NI 2014-15
We tend to think of the motorway as a thing or an object, something that has a singular function. Historically this is how it has been seen, with engineers designing bridges and embankments and suchlike with zeal … These objects like the M3 Urban Motorway, Belfast’s own Westway, are beautiful of course, but they have caused considerable damage to the city they were inflicted upon.

Actually, it’s the fact that we have seen the motorway as a solid object that has caused this problem. The motorway actually is a fluid and dynamic thing, and it should be seen as such: in fact it’s not an organ at all but actually tissue – something that connects rather than is. Once we start to see the motorway as tissue, it opens up new propositions about what the motorway is, is used for and does. This new dynamic and connective view unlocks the stasis of the motorway as edifice, and allows adaptation to happen: adaptation to old contexts that were ignored by the planners, and adaptation to new contexts that have arisen because of or in spite of our best efforts.

Motorways as tissue are more than just infrastructures: they are landscapes. These landscapes can be seen as surfaces on which flows take place, not only of cars, buses and lorries, but also of the globalized goods carried and the lifestyles and mobilities enabled. Here the infinite speed of urban change of thought transcends the declared speed limit [70 mph] of the motorway, in that a consignment of bananas can cause soil erosion in Equador, or the delivery of a new iphone can unlock connections and ideas the world over.

So what is this new landscape to be like? It may be a parallax-shifting, cognitive looking glass; a drone scape of energy transformation; a collective farm, or maybe part of a hospital. But what’s for sure, is that it is never fixed nor static: it pulses like a heartbeat through that most bland of landscapes, the countryside. It transmits forces like a Caribbean hurricane creating surf on an Atlantic Storm Beach: alien forces that mutate and re-form these places screaming into new, unclear and unintended futures.

And this future is clear: the future is urban. In this small rural country, motorways as tissue have made the whole of it: countryside, mountain, sea and town, into one singular, homogenous and hyper-connected, generic city.

Goodbye, place. Hello, surface!

Partial volume correction using bimodal contrast agents in PET-MRI

Tese de mestrado integrado em Engenharia Biomédica e Biofísica, apresentada à Universidade de Lisboa, através da Faculdade de Ciências, 2014

Analyse des paramètres atmosphériques des étoiles naines blanches dans le voisinage solaire

Ce mémoire présente une analyse homogène et rigoureuse de l’échantillon d’étoiles naines blanches situées à moins de 20 pc du Soleil. L’objectif principal de cette étude est d’obtenir un modèle statistiquement viable de l’échantillon le plus représentatif de la population des naines blanches. À partir de l’échantillon défini par Holberg et al. (2008), il a fallu dans un premier temps réunir le plus d’information possible sur toutes les candidates locales sous la forme de spectres visibles et de données photométriques. En utilisant les modèles d’atmosphère de naines blanches les plus récents de Tremblay & Bergeron (2009), ainsi que différentes techniques d’analyse, il a été permis d’obtenir, de façon homogène, les paramètres atmosphériques (Teff et log g) des naines blanches de cet échantillon. La technique spectroscopique, c.-à-d. la mesure de Teff et log g par l’ajustement des raies spectrales, fut appliquée à toutes les étoiles de notre échantillon pour lesquelles un spectre visible présentant des raies assez fortes était disponible. Pour les étoiles avec des données photométriques, la distribution d’énergie combinée à la parallaxe trigonométrique, lorsque mesurée, permettent de déterminer les paramètres atmosphériques ainsi que la composition chimique de l’étoile. Un catalogue révisé des naines blanches dans le voisinage solaire est présenté qui inclut tous les paramètres atmosphériques nouvellement determinés. L’analyse globale qui en découle est ensuite exposée, incluant une étude de la distribution de la composition chimique des naines blanches locales, de la distribution de masse et de la fonction luminosité.

Recherche et caractérisation des étoiles jeunes de faible masse dans le voisinage solaire

L'outil développé dans le cadre de cette thèse est disponible à l'adresse suivante: www.astro.umontreal.ca/~malo/banyan.php

Subpixel-Filterung für eine autostereoskopische Multiperspektiven-3-D-Darstellung hoher Qualität

Die stereoskopische 3-D-Darstellung beruht auf der naturgetreuen Präsentation verschiedener Perspektiven für das rechte und linke Auge. Sie erlangt in der Medizin, der Architektur, im Design sowie bei Computerspielen und im Kino, zukünftig möglicherweise auch im Fernsehen, eine immer größere Bedeutung. 3-D-Displays dienen der zusätzlichen Wiedergabe der räumlichen Tiefe und lassen sich grob in die vier Gruppen Stereoskope und Head-mounted-Displays, Brillensysteme, autostereoskopische Displays sowie echte 3-D-Displays einteilen. Darunter besitzt der autostereoskopische Ansatz ohne Brillen, bei dem N≥2 Perspektiven genutzt werden, ein hohes Potenzial. Die beste Qualität in dieser Gruppe kann mit der Methode der Integral Photography, die sowohl horizontale als auch vertikale Parallaxe kodiert, erreicht werden. Allerdings ist das Verfahren sehr aufwendig und wird deshalb wenig genutzt. Den besten Kompromiss zwischen Leistung und Preis bieten präzise gefertigte Linsenrasterscheiben (LRS), die hinsichtlich Lichtausbeute und optischen Eigenschaften den bereits früher bekannten Barrieremasken überlegen sind. Insbesondere für die ergonomisch günstige Multiperspektiven-3-D-Darstellung wird eine hohe physikalische Monitorauflösung benötigt. Diese ist bei modernen TFT-Displays schon recht hoch. Eine weitere Verbesserung mit dem theoretischen Faktor drei erreicht man durch gezielte Ansteuerung der einzelnen, nebeneinander angeordneten Subpixel in den Farben Rot, Grün und Blau. Ermöglicht wird dies durch die um etwa eine Größenordnung geringere Farbauflösung des menschlichen visuellen Systems im Vergleich zur Helligkeitsauflösung. Somit gelingt die Implementierung einer Subpixel-Filterung, welche entsprechend den physiologischen Gegebenheiten mit dem in Luminanz und Chrominanz trennenden YUV-Farbmodell arbeitet. Weiterhin erweist sich eine Schrägstellung der Linsen im Verhältnis von 1:6 als günstig. Farbstörungen werden minimiert, und die Schärfe der Bilder wird durch eine weniger systematische Vergrößerung der technologisch unvermeidbaren Trennelemente zwischen den Subpixeln erhöht. Der Grad der Schrägstellung ist frei wählbar. In diesem Sinne ist die Filterung als adaptiv an den Neigungswinkel zu verstehen, obwohl dieser Wert für einen konkreten 3-D-Monitor eine Invariante darstellt. Die zu maximierende Zielgröße ist der Parameter Perspektiven-Pixel als Produkt aus Anzahl der Perspektiven N und der effektiven Auflösung pro Perspektive. Der Idealfall einer Verdreifachung wird praktisch nicht erreicht. Messungen mit Hilfe von Testbildern sowie Schrifterkennungstests lieferten einen Wert von knapp über 2. Dies ist trotzdem als eine signifikante Verbesserung der Qualität der 3-D-Darstellung anzusehen. In der Zukunft sind weitere Verbesserungen hinsichtlich der Zielgröße durch Nutzung neuer, feiner als TFT auflösender Technologien wie LCoS oder OLED zu erwarten. Eine Kombination mit der vorgeschlagenen Filtermethode wird natürlich weiterhin möglich und ggf. auch sinnvoll sein.

Dental training system using haptic technology

In the U.K., dental students require to perform training and practice on real human tissues at the very early stage of their courses. Currently, the human tissues, such as decayed teeth, are mounted in a human head like physical model. The problems with these models in teaching are; (1) every student operates on tooth, which are always unique; (2) the process cannot be recorded for examination purposes and (3) same training are not repeatable. The aim of the PHATOM Project is to develop a dental training system using Haptic technology. This paper documents the project background, specification, research and development of the first prototype system. It also discusses the research in the visual display, haptic devices and haptic rendering. This includes stereo vision, motion parallax, volumetric modelling, surface remapping algorithms as well as analysis design of the system. A new volumetric to surface model transformation algorithm is also introduced. This paper includes the future work on the system development and research.

Cue combination for 3D location judgements

Cue combination rules have often been applied to the perception of surface shape but not to judgements of object location. Here, we used immersive virtual reality to explore the relationship between different cues to distance. Participants viewed a virtual scene and judged the change in distance of an object presented in two intervals, where the scene changed in size between intervals (by a factor of between 0.25 and 4). We measured thresholds for detecting a change in object distance when there were only 'physical' (stereo and motion parallax) or 'texture-based' cues (independent of the scale of the scene) and used these to predict biases in a distance matching task. Under a range of conditions, in which the viewing distance and position of the tarte relative to other objects was varied, the ration of 'physical' to 'texture-based' thresholds was a good predictor of biases in the distance matching task. The cue combination approach, which successfully accounts for our data, relies on quite different principles from those underlying geometric reconstruction.