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VaTEST : Validation of Transiting Exoplanets using Statistical Tools
VaTEST : Validation of Transiting Exoplanets using Statistical Tools
The VaTEST project was initiated at the beginning of May 2022 by Priyashkumar Mistry and Georgios Lekkas. This project's objective is to validate exoplanet signals by utilizing statistical tools and probabilistic algorithms in conjunction with other Python packages for the analysis of photometric and spectroscopic data. The work that will be done in the future on this project will be focused on the bulk validation of unconfirmed exoplanets. This will be accomplished through the use of a variety of statistical validation, false alarm and false positive diagnostic tests, as well as photometric and spectroscopic data analysis to calculate the exoplanet properties.
Statistical Analysis and Ephemeris Refinement of Exoplanets (Dissertation)
Statistical Analysis and Ephemeris Refinement of Exoplanets (Dissertation)
May 2022
In this work, we studied the different exoplanetary detection methods in detail. We also carried out a statistical analysis of all the confirmed Exoplanets using Python. The data is separated into four parts based on their detection facilities, i.e., Kepler, K2, Transiting Exoplanets Survey Satellite (TESS), and Other Facilities. The statistical analysis is based on the spectral types of host stars, apparent(V) magnitude of host stars, and radius of discovered exoplanets. We also calculated the occurrence rate of planets for Kepler & TESS satellites in different spectral types. The data here is collected from NASA Exoplanet Archive. As the HR diagram provides us a clear view of the stars with their Absolute Magnitudes, Temperatures, and Spectral types, its background information is essential because it provides a clear understanding of the stars and their properties. The amount of data is also essential because it helps us understand the stars in our galaxy and compare them, So this data is being used here to check the common properties of exoplanets’ host stars. We plotted the HR Diagram from data collected via the Hipparcos satellite to analyze the statistical outcomes and give the possible reasons behind those outcomes. Along with this analysis, we refine the ephemerides of 8 hot Jupiter exoplanets of WASP. Transit photometry data is collected from the TESS satellite available on the MAST archive, and Radial Velocity data is collected from published literature. We updated the planetary orbital period with a precision of 0.10 s and provided an updated Transit Epoch Time and other refined planetary & orbital parameters with high precision. Thus our work allows for accurate scheduling of future observations. Additionally, we observed the exoplanet target WASP-12b is going through the orbital decay with the rate of -28.201 ± 0.867 ms/yr due to the tidal evolution of a host star. We calculated the tidal quality factor Q to be 1.784 ×10⁵.
Link to the Report: Click Here
Link to the code (on GitHub): Click Here
Study of exoplanets
Study of exoplanets
December 2021
Dissertation Preliminaries Report attached below titled "Study of Exoplanets". In this project, I made a program using Python Packages LightKurve & Juliet to determine the planetary parameters from the observed data.
Link to the Report : Click Here
Link to the code (on GitHub) : Click Here
Simulation of Quantum Well structures using Octave
Simulation of Quantum Well structures using Octave
April 2021
A Quantum Well is essentially a potential well that has discrete energy levels. Quantum Wells are double heterostructures i.e. when two semiconductor materials are grown simultaneously into a sandwich. One very famous example of a double heterostructure that is an excellent example for the study of Quantum Well Structures is AlGaAs - GaAs. For purpose of this project, we shall stick to data of this structure for purpose of understanding the theory and logic of these programs. However, the program is designed keeping in mind all the basic physics of quantum well structures.
Group Project
Kavin Dave, Priyash Mistry, Zahabiyah Zaveri, Rahul Choudhury, Pujan Joshi
Report : Click Here
Link to the code (on GitHub) : Click Here
Report : Click Here
Study of Ocean Heat Content In the region of Arabian Ocean & Bay of Bengal
Study of Ocean Heat Content In the region of Arabian Ocean & Bay of Bengal
May 2021
Here I presented the Ocean Heat Content (OHC), at the two different regions of India, the Arabian Ocean & Bay of Bengal. The considered regions are on the same latitude. That is from 10 N to 20 N. The Longitude range for the Arabian Sea is considered from 60 E to 70 E, and for the Bay of Bengal is considered from 85 E to 95 E. Here we studied that how the OHC varies from the sea surface to depth. The satellite data for the same is collected from the Bhuvan ISRO website. The data of OHC is available for the different depths of 50 m, 100 m, 150 m, 200 m, 300 m, 500 m, and 700 m from the sea surface. This study shows that how the two different regions of oceans on the same Latitude have different kinds of OHC, and how it varies as we go from surface to depth and possible reasons for it.
Data Analysis of Hipparcos Catalog through Hetrzsprung Russel Diagram (HR Diagram)
Data Analysis of Hipparcos Catalog through Hetrzsprung Russel Diagram (HR Diagram)
April 2020
Here I plotted the HR Diagram using the data taken from Hipparcos Catalog. I used the following link to extract the necessary data from Hipparcos Catalog.
I had taken the data of the following region of a sky :
Data Range : HIP Number 44101 to 49100
Distance from Earth : 100 to 1000 Parsec
Horizontal Plane : 134.7478 to 150.3159 (degrees)
Vertical Plane : -89.7825 to -0.00098 (degrees)
Report : Click Here
Virtual Lab Experiment via Stellarium
Virtual Lab Experiment via Stellarium
April 2020
Virtual Lab Experiments to understand the different aspects of Astronomy via Stellarium application.
Report : Click Here
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