The PANDA experiment at FAIR is an antiproton experiment and it will offer unique possibilities for the study of hadron physics including hyperon physics. With the PANDA detector, it will be possible to exclusively reconstruct hyperon-antihyperon events. Hyperons are relatively long-lived particles (10−10s), which can travel for a distance of up to a few meters before decaying into their reconstructible decay products. In this project, I focus on the reaction p̅ p → Ξ̄+ Ξ− → Λ̅ π+ Λ π− → p̅ π+π+ p π− π−. The Ξ− (cascade) hyperons take a special role as they are the lightest hyperons to introduce a sequential decay topology, i.e., Ξ− → Λ π− → p π− π− (and c.c.). This constitutes a substantial challenge for the reconstruction algorithms. In this thesis, a Monte-Carlo simulation study of realistic track and event reconstruction of this Ξ̄+ Ξ− reaction in the region near the production threshold is done, and the event generation of the Ξ̄+ Ξ− reaction channel was performed by the EvtGen event generator in PandaRoot. For various realistic tracking algorithms, track and event reconstruction performance levels were investigated in PandaRoot.

The goal of the Q-weak experiment is to make a measurement of the proton's weak charge ($Q^p_W = 1-4\sin^2\theta_W$) to an accuracy of ~4%. This would represent a ~0.3% determination of the weak mixing angle ($\sin^2\theta_W$) at low energy. The measurement may be used for a precision test of the Standard Model (SM) prediction on the running of $\sin^2\theta_W$ with energy scale. The Q-weak experiment operates at Thomas Jefferson National Accelerator Facility (Jefferson Lab). The experiment determines the proton's weak charge by measuring the parity violating asymmetry in elastic electron-proton scattering at low momentum transfer $Q^2 = 0.026 (GeV/c)^2$ and forward angles (~8 degree). The anticipated size of the asymmetry, based on the SM, is about 230 parts per billion (ppb). With the proposed accuracy, the experiment may probe new physics beyond Standard Model at the TeV scale. This thesis focuses on my contributions to the experiment, including track reconstruction for momentum transfer determination of the scattering process, and the focal plane scanner, a detector I designed and built to measure the flux profile of scattered electrons on the focal plane of the Q-weak spectrometer to assist in the extrapolation of low beam current tracking results to high beam current. Preliminary results from the commissioning and the first run period of the Q-weak experiment are reported and discussed.

The goal of the Q-weak experiment is to make a measurement of the proton's weak charge ($Q^p_W = 1-4\sin^2\theta_W$) to an accuracy of ~4%. This would represent a ~0.3% determination of the weak mixing angle ($\sin^2\theta_W$) at low energy. The measurement may be used for a precision test of the Standard Model (SM) prediction on the running of $\sin^2\theta_W$ with energy scale. The Q-weak experiment operates at Thomas Jefferson National Accelerator Facility (Jefferson Lab). The experiment determines the proton's weak charge by measuring the parity violating asymmetry in elastic electron-proton scattering at low momentum transfer $Q^2 = 0.026 (GeV/c)^2$ and forward angles (~8 degree). The anticipated size of the asymmetry, based on the SM, is about 230 parts per billion (ppb). With the proposed accuracy, the experiment may probe new physics beyond Standard Model at the TeV scale. This thesis focuses on my contributions to the experiment, including track reconstruction for momentum transfer determination of the scattering process, and the focal plane scanner, a detector I designed and built to measure the flux profile of scattered electrons on the focal plane of the Q-weak spectrometer to assist in the extrapolation of low beam current tracking results to high beam current. Preliminary results from the commissioning and the first run period of the Q-weak experiment are reported and discussed.

The master´s thesis deals with the reconstruction design of Kyjov railway station. The solution is aimed at meeting the traffic requirements, modifying the layout of the platforms and access routes for the safe movement of people with reduced mobility and orientation. The proposal deals with rail crossing in accordance with current legislations. In this thesis is proposed renewal of drainage.

Das IceCube Neutrino Teleskop hat einen diffusen Fluss hochenergetischen astrophysikalischen Neutrinos entdeckten. Allerdings sind die Quellen die für die Mehrzahl der nachgewiesenen Neutrinos verantwortlich sind, noch unbekannt. Diese Arbeit untersucht die Möglichkeit, dass der beobachtete Neutrino-Fluss im Zentrum von aktiven galaktischen Kernen (AGN) erzeugt wird. Eine Stacking-Analyse wird durchgeführt, um die Korrelation zwischen verschiedenen Subpopulationen von AGN und hochenergetischen Neutrinos unter Verwendung von IceCube-Daten aus acht Jahren zu testen. AGN werden anhand ihrer Radioemission, Infrarot-Farbeigenschaften und ihres Röntgenflusses. Die Leuchtkraft der Akkretionsscheibe wird verwendet, um den Beitrag ausgewählter Galaxien zum Neutrinosignal zu gewichten. Die leuchtende AGN-Population trägt zu ~52% des von IceCube gemessenen diffusen Flusses bei 100 TeV mit einem Best-Fit-Spektralindex von 2 bei mit 2.83 sigma post-trial Signifikanz. Für die AGN-Probe mit geringer Leuchtkraft wird eine Signifikanz nach dem Versuch von nur 0.66 sigma gefunden, daher werden Obergrenzen festgelegt. Unter Annahme des Spektralindex für den astrophysikalischen Fluss von 2 und einer gleichverteilten gleiche Zusammensetzung Neutrinoflavour-Zusammensetzung auf der Erde, wird eine obere Flussgrenze berechnet, die den maximalen Beitrag der Kerne von AGN mit geringer Leuchtkraft zum diffusen TeV-PeV-Neutrino-Fluss auf ~51% bei 100 TeV beschränkt. Für diese Arbeit wurde auch eine neue Rekonstruktionsmethode entwickelt. In IceCube werden hochenergetische Myon-neutrinos durch die sekundären Myonen identifiziert, die durch Wechselwirkungen über geladene Ströme mit dem Eis erzeugt werden. In dem hier vorgestellten Rekonstruktionsschema wird die erwartete Ankunftszeitverteilung durch ein vorbestimmtes stochastisches Myon-Energieverlustprofil parametrisiert. Diese realistischere Parametrisierung führt zu einer Verbesserung der Myon-Winkelauflösung in IceCube um etwa 20%. / The IceCube neutrino telescope has measured a diffuse flux of high-energy astrophysical neutrinos. However, the sources responsible for the emission of the majority of the detected neutrinos are still unknown. The goal of this thesis is to explore the possibility that the neutrino flux observed by IceCube is produced in the cores of Active Galactic Nuclei (AGN). A stacking analysis is conducted to test for a correlation between various sub-populations of AGN and high-energy neutrinos using eight years of IceCube data. AGN are selected based on their radio emission, infrared color properties, and X-ray flux using the NVSS, AllWISE, ROSAT and XMMSL2 catalogs. The accretion disk luminosity estimated by the observed soft X-ray flux is used as a proxy for the contribution of selected galaxies to the neutrino signal. Two of the three AGN samples tested in this analysis show over-fluctuations, with the highest significance being of 2.83 sigma after trial correction. The luminous AGN population is found to contribute to ~52% of the diffuse flux measured by IceCube at 100 TeV with a best-fit spectral index of 2. For the low-luminosity AGN sample a post-trial significance of only 0.66 sigma is found, therefore upper limits are set. Assuming the spectral index for the astrophysical flux to be 2 and an equal composition of neutrino flavours arriving at Earth, an upper flux limit is calculated which constrains the maximal contribution of the cores of low-luminosity AGN to the diffuse TeV-PeV neutrino flux to be ~51% at 100 TeV. A new reconstruction method has also been developed for this thesis. In IceCube high-energy muon neutrinos are identified through the secondary muons produced via charge current interactions with the ice. In the reconstruction scheme presented in this thesis, the expected arrival time distribution is parameterized by a predetermined stochastic muon energy loss pattern, leading to an improvement of about 20% to the muon angular resolution of IceCube.

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