CCD Cameras
SLOAN ugriz Filters
One of the two standardized filter sets used for BRIEF projects, SLOAN ugriz is widely used due to its distinct, low-overlap response curves and generally flexible and efficient nature.
Linearity and Saturation
As inherent consequences of the design of CCD photon collection, pixel saturation and non-linearity are common challenges that must be carefully managed for effective scientific imaging.
Imaging Basics
This video serves as a best practices checklist for night sky imaging and outlines both the basic and more advanced methods involved with astronomical imaging.
Full Width Half Maximum
Used to determine the quality of your image, the Full Width Half Maximum (FWHM) process is used to determine the quality of images and is of particular importance in photometric and exoplanet research work. BRIEF primarily uses the OSS Pipeline to account for the FWHM process.
Camera Overview
Charged Coupled Devices (CCDs) are an integral part of astronomical imaging that utilize a matrix of electronically-measured photon counts to accurately represent an image.
UBVRI & JC filters
The UBVRI system covers all of the visual spectrum and some on the shorter and longer sides, and is the most commonly used system with a large network of standard stars.
Binning
Binning is a method of combining pixels on a CCD chip into one “super” pixel. This provides some advantages and disadvantages.
SNR
The signal-to-noise ratio (SNR) characterizes the quality of a measurement and determines the ultimate performance of the system. The three primary sources of noise in a CCD imaging system are photon noise, dark noise, and read noise, all of which must be considered in the SNR calculation.
FITS Files
FITS files are the end product of a CCD image of an astronomical object, and are designed to store data sets consisting of multi-dimensional arrays and 2-dimensional tables.
CCD Filters Overview
To get information from a target and make color pictures, filters are used. Filters block certain EM wavelengths.