Difference between revisions of "Bachelor Projects"
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=== Dark Matter === | === Dark Matter === | ||
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==== XENON1T - the world's most sensitive dark matter detector ==== | ==== XENON1T - the world's most sensitive dark matter detector ==== | ||
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The first goal of this project is to understand why dak matter is necessary to understand the universe, and how we could detect it with XENON1T. Then, you can contribute to our group's efforts preparing for | The first goal of this project is to understand why dak matter is necessary to understand the universe, and how we could detect it with XENON1T. Then, you can contribute to our group's efforts preparing for | ||
and analyzing the XENON1T data by, for example: examining XENON1T's calibration signals to check for problems in the experiment, testing our data analysis software with simulated dark matter signals, or studying the physics behind XENON1T's detection process to learn how to better distinguish dark matter signals from backgrounds. For data analyis, experience with or willingness to learn programming in python is essential. | and analyzing the XENON1T data by, for example: examining XENON1T's calibration signals to check for problems in the experiment, testing our data analysis software with simulated dark matter signals, or studying the physics behind XENON1T's detection process to learn how to better distinguish dark matter signals from backgrounds. For data analyis, experience with or willingness to learn programming in python is essential. | ||
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Supervisors: M.P. Decowski & J. Aalbers | Supervisors: M.P. Decowski & J. Aalbers | ||
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==== Neutrinoless double beta decay sensitivity study in future dark matter detectors ==== | ==== Neutrinoless double beta decay sensitivity study in future dark matter detectors ==== | ||
Revision as of 17:59, 8 February 2017
Bachelor Projects
Extreme Astronomy – Preparing for CTA, the Next-Generation Gamma-Ray Observatory
The Cherenkov Telescope Array (CTA) is a planned facility for measuring gamma rays from space covering more than four orders of magnitude in energy, up to energies exceeding 100 TeV. CTA employs the imaging atmospheric Cherenkov technique to measure properties of cosmic gamma rays. This technique is based on measuring Cherenkov light emitted during the development of a gamma-ray air shower. CTA will be built at two experimental sites, one in the Northern, one in the Southern hemisphere, and will consist of up to 100 telescopes. It represents a major leap forward in sensitivity and precision for gamma-ray astronomy, and will allow us to explore very-high-energy processes of the extreme Universe at an unprecedented level.
Two projects for students are available at the CTA group of UvA in the field of optical and photonic R&D contributing to the starting phase of CTA. For the first project the student will conduct measurements to characterise novel kinds of single-photon detectors, referred to as silicon photomultipliers, and evaluate different types of these sensors for their use for CTA. For the second project the student will develop and test an imaging system making use of a liquid crystal display. This flexible light source will be able to mimic images from different light sources of the night sky as seen by cameras of CTA, for instance gamma-ray air showers or stars, and will be used for camera tests and calibration.
Supervisors: David Berge, Maurice Stephan (postdoc)