Eine Referenzarchitektur für die assistierte und automatisierte Fahrzeugführung mit Fahrereinbindung

Gegenstand der Arbeit ist die Entwicklung einer funktionalen Systemarchitektur, die den Anforderungen des assistierten, teilautomatisierten bis hin zum vollautomatisierten Fahrens gerecht werden soll. Dabei steht insbesondere die Architektur als wissenschaftliche Disziplin im Vordergrund, in der Entscheidungsalternativen erarbeitet und durch Abwägung der sich daraus ergebenden Konsequenzen bewertet und dokumentiert werden. Im ersten Schritt erfolgt eine Anforderungsanalyse, in der die funktionalen Systemanforderungen in Form notwendiger Fahrmanöver hergeleitet sowie relevante nichtfunktionale Anforderungen (insbes. Test- und Erweiterbarkeit) an die Architektur identifiziert werden. Darauf aufbauend erfolgt die Entwicklung der Referenzarchitektur auf Basis hybrider Robotik-Basisarchitekturen, beginnend mit einer Festlegung des 3-Ebenen Fahrzeugführungsmodelles nach Donges als zugrunde liegendes hierarchisches Abstraktionsmodell. Von besonderer Bedeutung dabei ist das Zusammenspiel zwischen deliberativen Systemelementen zur Zielerreichung einerseits und reaktiven Systemelementen zur schnellen Reaktion auf sich ändernde Situationsparameter andererseits. Als Ergebnis liegt ein hierarchisches Mehrebenensystem mit vier Systemebenen vor. Neben der Festlegung der Kontrollhierarchie wird zusätzlich der Informationsbedarf der Planungsmodule in Richtung des Umfeldmodells skizziert sowie die notwendigen Mensch-Maschine-Schnittstellen zur Fahrereinbindung

The Galactic Mergers and Gravitational Unbound Populations

Motivated by the observations on the intra-cluster light (ICL) and inter-galactic stellar populations, n-body simulations are used to model the galactic merging events as a goal to investigate the production and distribution of gravitational unbound populations (GUPs). Both the parabolic and hyperbolic mergers are considered and each category includes six models with different relative orientations between two galaxies. Our results show that there are more (about a factor of two) GUP after a hyperbolic merging event than after a parabolic one. In general, depending on the relative orientation and also the relative velocity of the two galaxies in a merging pair, a head-on collision of a galaxy pair would only make a tiny fraction (less than one percent) of the initial stellar mass become luminous GUP but a considerable fraction (eight to fourteen percent) of the dark matter become dark GUP.Comment: 29 pages, 14 figures, published in MNRAS, Online Earl

Three-integral multi-component dynamical models and simulations of the nuclear star cluster in NGC 4244

Adaptive optics observations of the flattened nuclear star cluster in the nearby edge-on spiral galaxy NGC 4244 using the Gemini Near-Infrared Integral Field Spectrograph (NIFS) have revealed clear rotation. Using these kinematics plus 2MASS photometry we construct a series of axisymmetric two-component particle dynamical models with our improved version of NMAGIC, a flexible Chi^2-made-to-measure code. The models consist of a nuclear cluster disc embedded within a spheroidal particle population. We find a mass for the nuclear star cluster of M=1.6^+0.5_-0.2 x 10^7 M_sun within ~42.4 pc (2"). We also explore the presence of an intermediate mass black hole and show that models with a black hole as massive as M_bh = 5.0 x 10^5 M_sun are consistent with the available data. Regardless of whether a black hole is present or not, the nuclear cluster is vertically anisotropic (beta_z < 0), as was found with earlier two-integral models. We then use the models as initial conditions for N-body simulations. These simulations show that the nuclear star cluster is stable against non-axisymmetric perturbations. We also explore the effect of the nuclear cluster accreting star clusters at various inclinations. Accretion of a star cluster with mass 13% that of the nuclear cluster is already enough to destroy the vertical anisotropy, regardless of orbital inclination.Comment: Replaced with the version accepted for publication in MNRAS. 13 pages, 10 figures, 3 table

Galaxy Assembly Bias on the Red Sequence

Using samples drawn from the Sloan Digital Sky Survey, we study the relationship between local galaxy density and the properties of galaxies on the red sequence. After removing the mean dependence of average overdensity (or "environment") on color and luminosity, we find that there remains a strong residual trend between luminosity-weighted mean stellar age and environment, such that galaxies with older stellar populations favor regions of higher overdensity relative to galaxies of like color and luminosity (and hence of like stellar mass). Even when excluding galaxies with recent star-formation activity (i.e., younger mean stellar ages) from the sample, we still find a highly significant correlation between stellar age and environment at fixed stellar mass. This residual age-density relation provides direct evidence for an assembly bias on the red sequence such that galaxies in higher-density regions formed earlier than galaxies of similar mass in lower-density environments. We discuss these results in the context of the age-metallicity degeneracy and in comparison to previous studies at low and intermediate redshift. Finally, we consider the potential role of assembly bias in explaining recent results regarding the evolution of post-starburst (or post-quenching) galaxies and the environmental dependence of the type Ia supernova rate.Comment: Accepted for publication in MNRA

How do minor mergers promote inside-out growth of ellipticals, transforming the size, density profile and dark matter fraction?

There is observational evidence for inside-out growth of elliptical galaxies since $z \gtrsim 2-3$, which is not driven by in-situ star formation. Many systems at high redshift have small sizes $\sim 1kpc$ and surface brightness profiles with low Sersic indices n. The most likely descendants have, on average, grown by a factor of two in mass and a factor of four in size, indicating $r \propto M^{\alpha}$ with $\alpha \gtrsim 2$. They also have surface brightness profiles with $n \gtrsim 5$. This evolution can be qualitatively explained on the basis of two assumptions: compact ellipticals predominantly grow by collisionless minor or intermediate 'dry' mergers, and they are embedded in massive dark matter halos. We draw these conclusions from idealized collisionless mergers spheroidal galaxies - with and without dark matter - with mass ratios of 1:1, 1:5, and 1:10. The sizes evolve as $r \propto M^{\alpha}$ with $\alpha < 2$ for mass-ratios of 1:1. For minor mergers of galaxies embedded in dark matter halos, the sizes grow significantly faster and the profile shapes change more rapidly. Mergers with moderate mass-ratios of 1:5 give $\alpha \sim 2.3$ and a final Sersic index of $n = 9.5$ after doubling the stellar mass. This is accompanied by a significant increase of the dark matter fraction within the stellar half-mass radius, driven by the strong size increase probing larger, dark matter dominated regions. Only a few intermediate mass-ratio mergers of galaxies embedded in massive dark matter halos can result in the observed concurrent inside-out growth and the rapid evolution in profile shapes. Apart from negative stellar metallicity gradients such a 'minor' merger scenario also predicts significantly lower dark matter fractions for $z \sim 2$ compact quiescent galaxies and their rare present day analogues (abbreviated).Comment: accepted for publicatio

EuReCa ONE—27 Nations, ONE Europe, ONE Registry A prospective one month analysis of out-of-hospital cardiac arrest outcomes in 27 countries in Europe

AbstractIntroductionThe aim of the EuReCa ONE study was to determine the incidence, process, and outcome for out of hospital cardiac arrest (OHCA) throughout Europe.MethodsThis was an international, prospective, multi-centre one-month study. Patients who suffered an OHCA during October 2014 who were attended and/or treated by an Emergency Medical Service (EMS) were eligible for inclusion in the study. Data were extracted from national, regional or local registries.ResultsData on 10,682 confirmed OHCAs from 248 regions in 27 countries, covering an estimated population of 174 million. In 7146 (66%) cases, CPR was started by a bystander or by the EMS. The incidence of CPR attempts ranged from 19.0 to 104.0 per 100,000 population per year. 1735 had ROSC on arrival at hospital (25.2%), Overall, 662/6414 (10.3%) in all cases with CPR attempted survived for at least 30 days or to hospital discharge.ConclusionThe results of EuReCa ONE highlight that OHCA is still a major public health problem accounting for a substantial number of deaths in Europe.EuReCa ONE very clearly demonstrates marked differences in the processes for data collection and reported outcomes following OHCA all over Europe. Using these data and analyses, different countries, regions, systems, and concepts can benchmark themselves and may learn from each other to further improve survival following one of our major health care events

Tides in colliding galaxies

Long tails and streams of stars are the most noticeable upshots of galaxy collisions. Their origin as gravitational, tidal, disturbances has however been recognized only less than fifty years ago and more than ten years after their first observations. This Review describes how the idea of galactic tides emerged, in particular thanks to the advances in numerical simulations, from the first ones that included tens of particles to the most sophisticated ones with tens of millions of them and state-of-the-art hydrodynamical prescriptions. Theoretical aspects pertaining to the formation of tidal tails are then presented. The third part of the review turns to observations and underlines the need for collecting deep multi-wavelength data to tackle the variety of physical processes exhibited by collisional debris. Tidal tails are not just stellar structures, but turn out to contain all the components usually found in galactic disks, in particular atomic / molecular gas and dust. They host star-forming complexes and are able to form star-clusters or even second-generation dwarf galaxies. The final part of the review discusses what tidal tails can tell us (or not) about the structure and content of present-day galaxies, including their dark components, and explains how tidal tails may be used to probe the past evolution of galaxies and their mass assembly history. On-going deep wide-field surveys disclose many new low-surface brightness structures in the nearby Universe, offering great opportunities for attempting galactic archeology with tidal tails.Comment: 46 pages, 13 figures, Review to be published in "Tidal effects in Astronomy and Astrophysics", Lecture Notes in Physics. Comments are most welcom

Eine Referenzarchitektur für die assistierte und automatisierte Fahrzeugführung mit Fahrereinbindung

Gegenstand der Arbeit ist die Entwicklung einer funktionalen Systemarchitektur, die den Anforderungen des assistierten, teilautomatisierten bis hin zum vollautomatisierten Fahrens gerecht werden soll. Dabei steht insbesondere die Architektur als wissenschaftliche Disziplin im Vordergrund, in der Entscheidungsalternativen erarbeitet und durch Abwägung der sich daraus ergebenden Konsequenzen bewertet und dokumentiert werden. Im ersten Schritt erfolgt eine Anforderungsanalyse, in der die funktionalen Systemanforderungen in Form notwendiger Fahrmanöver hergeleitet sowie relevante nichtfunktionale Anforderungen (insbes. Test- und Erweiterbarkeit) an die Architektur identifiziert werden. Darauf aufbauend erfolgt die Entwicklung der Referenzarchitektur auf Basis hybrider Robotik-Basisarchitekturen, beginnend mit einer Festlegung des 3-Ebenen Fahrzeugführungsmodelles nach Donges als zugrunde liegendes hierarchisches Abstraktionsmodell. Von besonderer Bedeutung dabei ist das Zusammenspiel zwischen deliberativen Systemelementen zur Zielerreichung einerseits und reaktiven Systemelementen zur schnellen Reaktion auf sich ändernde Situationsparameter andererseits. Als Ergebnis liegt ein hierarchisches Mehrebenensystem mit vier Systemebenen vor. Neben der Festlegung der Kontrollhierarchie wird zusätzlich der Informationsbedarf der Planungsmodule in Richtung des Umfeldmodells skizziert sowie die notwendigen Mensch-Maschine-Schnittstellen zur Fahrereinbindung