New Observations of Balmer Continuum Flux in Solar Flares:Instrument Description and First Results

Increase in the Balmer continuum radiation during solar flares was predicted by various authors, but has never been firmly confirmed observationally using ground-based slit spectrographs. Here we describe a new post-focal instrument, the image selector, with which the Balmer continuum flux can be measured from the whole flare area, in analogy to successful detections of flaring dMe stars. The system was developed and put into operation at the horizontal solar telescope HSFA2 of the Ondřejov Observatory. We measure the total flux by a fast spectrometer from a limited but well-defined region on the solar disk. Using a system of diaphragms, the disturbing contribution of a bright solar disk can be eliminated as much as possible. Light curves of the measured flux in the spectral range 350 – 440 nm are processed, together with the Hα images of the flaring area delimited by the appropriate diaphragm. The spectral flux data are flat-fielded, calibrated, and processed to be compared with model predictions. Our analysis of the data proves that the described device is sufficiently sensitive to detect variations in the Balmer continuum during solar flares. Assuming that the Balmer-continuum kernels have at least a similar size as those visible in Hα, we find the flux increase in the Balmer continuum to reach 230 – 550 % of the quiet continuum during the observed X-class flare. We also found temporal changes in the Balmer continuum flux starting well before the onset of the flare in Hα.

Spectral analysis of four 'hypervariable' AGN: a micro-needle in the haystack?

We analyze four extreme AGN transients to explore the possibility that they are caused by rare, high-amplitude microlensing events. These previously unknown type-I AGN are located in the redshift range 0.6-1.1 and show changes of > 1.5 magnitudes in the g-band on a timescale of ~years. Multi-epoch optical spectroscopy, from the William Herschel Telescope, shows clear differential variability in the broad line fluxes with respect to the continuum changes and also evolution in the line profiles. In two cases a simple point-source, point-lens microlensing model provides an excellent match to the long-term variability seen in these objects. For both models the parameter constraints are consistent with the microlensing being due to an intervening stellar mass object but as yet there is no confirmation of the presence of an intervening galaxy. The models predict a peak amplification of 10.3/13.5 and an Einstein timescale of 7.5/10.8 years respectively. In one case the data also allow constraints on the size of the CIII] emitting region, with some simplifying assumptions, to to be ~1.0-6.5 light-days and a lower limit on the size of the MgII emitting region to be > 9 light-days (half-light radii). This CIII] radius is perhaps surprisingly small. In the remaining two objects there is spectroscopic evidence for an intervening absorber but the extra structure seen in the lightcurves requires a more complex lensing scenario to adequately explain.

The Little Galaxies That Could Reionize the Universe

Thesis (Ph.D.)--University of Washington, 2016-08

Histoire évolutive de la galaxie spirale NGC 5430

La galaxie spirale barrée NGC 5430 est particulière en ce sens qu’elle présente un noeud Wolf-Rayet très lumineux et des bras asymétriques. Des spectres longue-fente le long de la barre et dans le bras déformé ainsi que des données SpIOMM couvrant l’ensemble de la galaxie ont été analysées. L’absorption stellaire sous-jacente a été soustraite des spectres longue-fente à l’aide d’un ajustement de modèles théoriques de populations stellaires fait avec le programme GANDALF. L’absorption a un impact très important sur le calcul de l’extinction ainsi que sur les différents diagnostics propres aux régions HII et aux populations stellaires jeunes. Enfin, cette étude montre que NGC 5430 comporte une composante gazeuse ionisée diffuse sur toute son étendue et qu’il est important d’en tenir compte afin d’appliquer correctement les diagnostics. Un des scénarios évolutifs proposés au terme de cette étude est que le noeud Wolf-Rayet constitue le restant d’une petite galaxie ou d’un nuage intergalactique qui serait entré en collision avec NGC 5430. Une structure englobant le noeud Wolf-Rayet se déplace à une vitesse considérablement inférieure (50 - 70 km s-1) à celle attendue à une telle distance du centre de la galaxie (200 - 220 km s-1). De plus, le noeud Wolf-Rayet semble très massif puisque l’intensité maximale du continu stellaire de cette région est semblable à celle du noyau et est de loin supérieure à celle de l’autre côté de la barre. Le nombre d’étoiles Wolf-Rayet (2150) est aussi considérable. Il n’est toutefois pas exclu que la différence de vitesses observée témoigne d’un écoulement de gaz le long de la barre, qui alimenterait la formation stellaire du noeud Wolf-Rayet ou du noyau.

De la métallicité et la formation stellaire des galaxies spirales barrées

Afin d’étudier l’historique de formation stellaire et d’enrichissement chimique des galaxies spirales barrées, j’ai simulé l’évolution de 27 galaxies spirales, barrées et non barrées, de diverses masses stellaires et fractions de gaz. Alors que les galaxies non barrées présentent une évolution lente et continue sur les deux milliards d’années que durent nos simulations, les galaxies barrées ont une évolution bien plus explosive, et ce particulièrement pour les galaxies les plus massives. Dans un premier temps, je montre que la présence de la barre entraine un flot important de gaz des régions périphériques vers le centre de la galaxie barrée, causant un sursaut de formation stellaire et une croissance importante de l’abondance chimique centrale, et que l’amplitude et la vitesse à laquelle ce sursaut arrive augmentent avec la masse de la galaxie. Cet épisode de sursaut stellaire entraine alors une diminution importante de la masse de gaz, entrainant à son tour une décroissance de la formation stellaire et une stagnation de l’enrichissement chimique pour le reste de l’évolution de la galaxie. Dans un deuxième temps, je montre qu’à cause de la dynamique en deux périodes très différentes des galaxies barrées, deux galaxies de masse très semblable peuvent avoir des taux de formation stellaire et des métallicités complètement différentes en fonction de leur stade évolutif, stade qu’on ne peut déterminer aisément. Cette difficulté est tout aussi importante lorsqu’on compare le coeur des galaxies barrées et non barrées entre elles, étant donné que des coeurs comparables sont situés dans les galaxies très différentes, et que des galaxies semblables ont des coeurs très différents.

Le continuum des violences genrées dans les trajectoires migratoires des Colombiennes en situation de refuge en Équateur

La migration internationale, expérience centrale et de plus en plus féminisée de la mondialisation, semble fortement structurée par les rapports de genre qui peuvent faciliter ou limiter la trajectoire. En outre, une attention particulière doit être portée à la vulnérabilité différenciée des femmes face aux violences dans les processus de recrutement, de déplacement et de passage des frontières. Le contexte de déplacement forcé en étant un particulier, il est essentiel de prendre en compte la situation et le point de vue des femmes en situation de refuge tout comme il est nécessaire de questionner les structures mises en place pour assurer leur accès aux services ainsi que le respect de leurs droits. Dans ce contexte, cette recherche s’intéresse à l’importance de l’interaction entre les différents axes d’inégalités sociales dans la production et la transformation des formes de violences basées sur le genre vécues par les déplacées colombiennes tant dans la phase prédépart, dans l’étape de déplacement que lors de leur insertion dans le pays voisin où elles cherchent refuge : l’Équateur. En plus de s’amalgamer aux autres axes de différenciation sociale tels que l’âge, l’ethnie, la classe sociale et l’orientation sexuelle les caractéristiques vulnérabilisantes liées au genre se dévoilent dans un continuum de violences qui vient à son tour influencer les rapports inégaux. L’utilisation d’un concept comme celui du continuum permet une réflexion sur la nature multi-facétique de la violence. En plus d’aller plus loin que la hiérarchisation des abus, ce concept favorise l’exploration de formes de violences qui, contrairement aux violences extrêmes et directes, sont moins communément étudiées. En effet, les violences basées sur le genre ne sont pas des phénomènes isolés, mais des manifestations qui s’entrecroisent le long d’un continuum au cours duquel elles se supportent, se nourrissent mutuellement et parfois se fusionnent pour se transformer.

David Phillips: The German example, English interest in educational provision in Germany since 1800, London / New York: Continuum 2011 [Rezension]

David Phillips: The German Example, English Interest in Educational Provision in Germany Since 1800, London / New York: Continuum 2011 (230 S.; ISBN 978-1-44114-130-9; 70,00 EUR)

Structure morphologique et populations stellaires d’un échantillon de galaxies spirales

Afin de caractériser la structure morphologique et les populations stellaires d’un échantillon de treize galaxies spirales, j’ai analysé des images WISE et GALEX, et j’ai construit des diagrammes magnitude-magnitude et couleur-magnitude pixel à pixel. Les diagrammes présentent des groupes de pixels qui correspondent spatialement aux composantes structurales des galaxies. Les diagrammes ainsi que les profils radiaux de brillance de surface indiquent que les variations de la densité surfacique de masse de la vieille population stellaire jouent un rôle important dans la différenciation des structures. On estime l’âge des jeunes complexes stellaires et l’extinction dans ces galaxies en les comparant à des modèles de populations stellaires simples nées de sursauts de formation stellaire instantanée. L’étude de ces propriétés est possible grâce à la combinaison des données ultraviolettes et infrarouge et à la grande sensibilité de la couleur ultraviolette à la variation de l’âge. On observe un gradient d’extinction dont la pente est liée à la présence d’une barre ou d’une activité nucléaire : en effet, l’extinction décroît avec la distance galactocentrique et la pente est plus petite pour les galaxies ayant une barre ou une activité nucléaire. On observe également un gradient d’âge où les régions externes sont moins évoluées que celles du centre sauf pour les galaxies de type tardif.

Exploring the cardiovascular disease continuum: blood pressure and target organ damage

Introduction The objectives of this thesis are to: (1) examine how ambulatory blood pressure monitoring (ABPM) refines office blood pressure (BP) measurement; (2) determine if absolute ambulatory BP or dipping status is better associated with target organ damage (TOD); (3) explore the association of isolated nocturnal hypertension (INH) with TOD; and (4) investigate the association of night-time BP with ultrasound markers of cardiovascular damage. Methods Data from the Mitchelstown Cohort Study was analysed to deliver objectives 1 and 2. Objective 3 was addressed by a systematic review and analysis of data from the Mitchelstown Study. A sample of participants from the Mitchelstown Study underwent an echocardiogram for speckle tracking analysis and carotid ultrasound to achieve objective 4. Results ABPM reclassifies hypertension status in approximately a quarter of individuals, with white coat and masked hypertension prevalence rates of 11% and 13% respectively. Night-time systolic BP is better associated with TOD than daytime systolic BP and dipping level. In multi-variable models the odds ratio (OR) for LVH was 1.4 (95% CI 1.1 -1.8) and for albumin:creatinine ratio ≥ 1.1 mg/mmol was 1.5 (95% CI 1.2 – 1.8) for each 10 mmHg rise in night-time systolic BP. The evidence for the association of INH with TOD is inconclusive. Night-time systolic BP is significantly associated with global longitudinal strain (GLS) (beta coefficient 0.85 for every 10 mmHg rise, 95% CI 0.3 – 1.4) and carotid plaques (OR 1.9 for every 10 mmHg rise, 95% CI 1.1 – 3.2) in univariable analysis. The findings persist for GLS in sex and age adjusted models but not in multivariable models. Discussion Hypertension cannot be effectively managed without using ABPM. Night-time systolic BP is better associated with TOD than daytime systolic BP and dipping level, and therefore, may be a better therapeutic target in future studies.

Nuclei of Nearby Active Galaxies: NIR and Sub-mm Views and Finalizing the LINC-NIRVANA Fringe and Flexure Tracking System: Flexure and Temperature Behavior

The work presented in my thesis addresses the two cornerstones of modern astronomy: Observation and Instrumentation. Part I deals with the observation of two nearby active galaxies, the Seyfert 2 galaxy NGC 1433 and the Seyfert 1 galaxy NGC 1566, both at a distance of $\sim10$ Mpc, which are part of the Nuclei of Galaxies (NUGA) sample. It is well established that every galaxy harbors a super massive black hole (SMBH) at its center. Furthermore, there seems to be a fundamental correlation between the stellar bulge and SMBH masses. Simulations show that massive feedback, e.g., powerful outflows, in Quasi Stellar Objects (QSOs) has an impact on the mutual growth of bulge and SMBH. Nearby galaxies follow this relation but accrete mass at much lower rates. This gives rise to the following questions: Which mechanisms allow feeding of nearby Active Galactic Nuclei (AGN)? Is this feeding triggered by events, e.g., star formation, nuclear spirals, outflows, on $\sim500$ pc scales around the AGN? Does feedback on these scales play a role in quenching the feeding process? Does it have an effect on the star formation close to the nucleus? To answer these questions I have carried out observations with the Spectrograph for INtegral Field Observation in the Near Infrared (SINFONI) at the Very Large Telescope (VLT) situated on Cerro Paranal in Chile. I have reduced and analyzed the recorded data, which contain spatial and spectral information in the H-band ($1.45 \mic-1.85 \mic$) and K-band ($1.95 \mic-2.45 \mic$) on the central $10\arcsec\times10\arcsec$ of the observed galaxies. Additionally, Atacama Large Millimeter/Sub-millimeter Array (ALMA) data at $350$ GHz ($\sim0.87$ mm) as well as optical high resolution Hubble Space Telescope (HST) images are used for the analysis. For NGC 1433 I deduce from comparison of the distributions of gas, dust, and intensity of highly ionized emission lines that the galaxy center lies $\sim70$ pc north-northwest of the prior estimate. A velocity gradient is observed at the new center, which I interpret as a bipolar outflow, a circum nuclear disk, or a combination of both. At least one dust and gas arm leads from a $r\sim200$ pc ring towards the nucleus and might feed the SMBH. Two bright warm H$_2$ gas spots are detected that indicate hidden star formation or a spiral arm-arm interaction. From the stellar velocity dispersion (SVD) I estimate a SMBH mass of $\sim1.74\times10^7$ \msol. For NGC 1566 I observe a nuclear gas disk of $\sim150$ pc in radius with a spiral structure. I estimate the total mass of this disk to be $\sim5.4\times10^7$ \msol. What mechanisms excite the gas in the disk is not clear. Neither can the existence of outflows be proven nor is star formation detected over the whole disk. On one side of the spiral structure I detect a star forming region with an estimated star formation rate of $\sim2.6\times10^{-3}$ \msol\ yr$^{-1}$. From broad Br$\gamma$ emission and SVD I estimate a mean SMBH mass of $\sim5.3\times10^6$ \msol\ with an Eddington ratio of $\sim2\times10^{-3}$. Part II deals with the final tests of the Fringe and Flexure Tracker (FFTS) for LBT INterferometric Camera and the NIR/Visible Adaptive iNterferometer for Astronomy (LINC-NIRVANA) at the Large Binocular Telescope (LBT) in Arizona, USA, which I conducted. The FFTS is the subsystem that combines the two separate beams of the LBT and enables near-infrared interferometry with a significantly large field of view. The FFTS has a cryogenic system and an ambient temperature system which are separated by the baffle system. I redesigned this baffle to guarantee the functionality of the system after the final tests in the Cologne cryostat. The redesign did not affect any scientific performance of LINC-NIRVANA. I show in the final cooldown tests that the baffle fulfills the temperature requirement and stays $<110$ K whereas the moving stages in the ambient system stay $>273$ K, which was not given for the old baffle design. Additionally, I test the tilting flexure of the whole FFTS and show that accurate positioning of the detector and the tracking during observation can be guaranteed.

Modelling continuum mechanics phenomena using three dimensional unstructured meshes on massively parallel processors

The difficulties encountered in implementing large scale CM codes on multiprocessor systems are now fairly well understood. Despite the claims of shared memory architecture manufacturers to provide effective parallelizing compilers, these have not proved to be adequate for large or complex programs. Significant programmer effort is usually required to achieve reasonable parallel efficiencies on significant numbers of processors. The paradigm of Single Program Multi Data (SPMD) domain decomposition with message passing, where each processor runs the same code on a subdomain of the problem, communicating through exchange of messages, has for some time been demonstrated to provide the required level of efficiency, scalability, and portability across both shared and distributed memory systems, without the need to re-author the code into a new language or even to support differing message passing implementations. Extension of the methods into three dimensions has been enabled through the engineering of PHYSICA, a framework for supporting 3D, unstructured mesh and continuum mechanics modeling. In PHYSICA, six inspectors are used. Part of the challenge for automation of parallelization is being able to prove the equivalence of inspectors so that they can be merged into as few as possible.

On the continuum modelling of granular flows with the aid of micro-mechanical parametrisations

Abstract not available

Topology Optimization of continuum structures with epsilon-relaxed stress constraints

Topology optimization of linear elastic continuum structures is a challenging problem when considering local stress constraints. The reasons are the singular behavior of the constraint with the density design variables, combined with the large number of constraints even for small finite element meshes. This work presents an alternative formulation for the s-relaxation technique, which provides an workaround for the singularity of the stress constraint. It also presents a new global stress constraint formulation. Derivation of the sensitivities for the constraint by the adjoint method is shown. Results for single and multiple load cases show the potential of the new formulation.

Continuum tensor network field states, path integral representations and spatial symmetries

A natural way to generalize tensor network variational classes to quantum field systems is via a continuous tensor contraction. This approach is first illustrated for the class of quantum field states known as continuous matrix-product states (cMPS). As a simple example of the path-integral representation we show that the state of a dynamically evolving quantum field admits a natural representation as a cMPS. A completeness argument is also provided that shows that all states in Fock space admit a cMPS representation when the number of variational parameters tends to infinity. Beyond this, we obtain a well-behaved field limit of projected entangled-pair states (PEPS) in two dimensions that provide an abstract class of quantum field states with natural symmetries. We demonstrate how symmetries of the physical field state are encoded within the dynamics of an auxiliary field system of one dimension less. In particular, the imposition of Euclidean symmetries on the physical system requires that the auxiliary system involved in the class' definition must be Lorentz-invariant. The physical field states automatically inherit entropy area laws from the PEPS class, and are fully described by the dissipative dynamics of a lower dimensional virtual field system. Our results lie at the intersection many-body physics, quantum field theory and quantum information theory, and facilitate future exchanges of ideas and insights between these disciplines.