Creating A Fitting Function for Exoplanet Detection

Abstract

Rough Copy, will be revised later on: The purpose of this project is to create an accurate fitting function for transiting stars. Data from these transiting stars will ultimately be used to identify new exoplanets. It is very apparent that a fitting function that addresses multiple environmental parameters affecting brightness measurements is needed as exoplanet identification can be a cumbersome and time consuming process. Utilizing computer code will streamline the process of exoplanet identification and can then allow researchers to focus their energies solely on data collection. It should be duly noted that in order to collect data from transiting stars; one can use amateur equipment but, for the sake of maximum accuracy; a high powered telescope would be more suitable (“Exoplanet Transit Parameters”, 2008). Previous students at Macewan that collected transiting star data utilized the Athabasca University Robotic Telescope (AURT) (“Defining the Transit Method”, 2017). This telescope requires booking periods thus, in order to maximize utility and efficiency; more energy should be spent on data collection and result analysis.

Discipline: Physical Sciences

Faculty Mentor: Dr. Stefan Cartledge