Filtering by
star formation (Dahlem et al. 2006) by comparing maps of 120-240 MHz synchrotron emission and hydrogen alpha (Hα) emission of the tidally-interacting, edge-on, barred spiral galaxy UGC 9665. Synchrotron emission traces magnetic field strength to a rough first order, while Hα emission traces recent massive star formation. UGC 9665 was selected because it was included in the LOw Frequency ARray (LOFAR) TwoMetre Sky Survey (LoTSS; Shimwell et al. (2017)) as well as the Calar Alto Legacy Integral Field Area Survey (CALIFA; Sanchez et al. (2012)). I generated vertical intensity profiles at several distances along the disk from the galactic center for synchrotron emission and Hα in order to measure how the intensity of each falls off with distance from the midplane. In addition to correlating the vertical profiles to see if there is a relationship between star formation and magnetic field strength, I fit the LOFAR vertical profiles to characteristic Gaussian and exponential functions given by Dumke et al. (1995). Fitting these equations have been shown to be good indicators of the main mode of cosmic ray transport, whether it is advection (exponential fit) or diffusion (Gaussian fit) (Heesen et al. 2016). Cosmic rays originate from supernova,
and core collapse supernovae occur in star forming regions, which also produce
advective winds, so I test the correlation between star-forming regions and advective regions as predicted by the Heesen et al. (2016) method. Similar studies should be conducted on different galaxies in the future in order to further test these hypotheses and how well LOFAR and CALIFA complement each other, which will be made possible by the full release of the LOFAR Two-Metre Sky Survey (LoTSS) (Shimwell et al. 2017).
As part of NASA’s Artemis program, NASA intends to construct the Lunar Gateway space station in a near rectilinear halo orbit (NRHO) about the L2 Lagrange point of the Earth-Moon system in the near future. Gateway will help facilitate astronaut landings on the surface of the Moon and support numerous scientific endeavors. One of these scientific endeavors is FARSIDE. FARSIDE is a radio telescope array concept that will be deployed on the surface of the far side of the moon. Because of this, FARSIDE will require an orbiter, such as Gateway, to act as a communication relay to be able to communicate with ground stations on Earth. This thesis analyzes how the Lunar Gateway space station can assist FARSIDE with its communication with Earth and how unintentionally scattered radio signals from FARSIDE could affect the telescope’s astronomical observations. It provides insight into the optimal deployment latitude on the lunar surface for FARSIDE. The thesis first begins with a literature review of the circular restricted three body problem (CR3BP) and halo orbit calculations. This is followed by an analysis of an example halo orbit for the distance, elevation angle, and azimuth angle it has viewed from two possible sites for FARSIDE over one period of its trajectory. Using this same approach, an analysis of the Lunar Gateway’s NRHO trajectory over one year was performed along with an analysis of the scattered radio flux from ground stations on Earth and the flux leakage from Gateway. Three different possible deployment latitudes for FARSIDE were investigated: the equator, 30 degrees, and -30 degrees. The analysis in this thesis ultimately showed that a deployment latitude below the equator would be the preferable choice to maximize the visibility of Lunar Gateway from FARSIDE considering the geometry of the Lunar Gateway’s orbit.