CHAPTER TIMESTAMPS<br />---------------------------------------<br />00:00:00 Introduction<br />00:00:10 Mask Particual pIxel<br />00:16:27 Mask Pixel Above Threshold Intensity Value<br />00:29: 51 Rectangular Masking<br />00:41: 33 Elliptical/Circular Masking<br />01:00:33 Elliptical Annlus Masking <br />01:08:44 MASK FITS Spectra<br />01:28:31 MASK Spectral Data Cube<br /><br />FITS (Flexible Image Transport System) is the standard file format used in astronomy for storing and analyzing data. Let’s break it down:<br /><br />FITS Images: These are 2D arrays that show images of the sky, where each pixel represents light intensity from a specific point in space.<br />Spectra: Spectral data reveals how light intensity changes across different wavelengths, providing insights into the composition, temperature, and motion of celestial objects.<br />Data Cubes: These are 3D datasets that combine spatial and spectral information. Imagine a stack of 2D images, each corresponding to a specific wavelength, forming a "cube" of data.<br />Masking: In this context, masking is a technique used to isolate or exclude specific parts of the data. For example:<br /><br />In FITS images, masking can be applied to remove noisy or invalid pixels, such as those caused by cosmic rays or defective detectors.<br />For spectra and data cubes, masking might exclude wavelengths or regions with interference or noise, ensuring the analysis focuses only on reliable data.<br />Masking is a critical step in cleaning and preparing astronomical data, allowing researchers to focus on the most meaningful parts of their observations.
