Photometry
Flow of A Photometry Project
This lesson discusses the basic outline and design of a photometry project from identification of an object to the final stages of measurement and analysis.
Calculating Magnitude
This lesson explains how to utilize aperture photometry to calculate the magnitude of a given object.
APASS
The AAVSO Photometric All-Sky Survey (APASS) is a key all-sky survey that helps various research programs measure, adjust, and standardize their photometric systems.
Point Spread Function (PSF)
Point Spread Function (PSF) uses known optical behaviors of both stellar light and the imaging system to decrease the complexity of images and create visual separation between objects for more accurate study.
Aperture Photometry
Aperture Photometry, key to all studies in photometry, is one of the two most common methods of measuring the flux output of a star and is the most accurate when used with non-crowded images.
Photometry an Overview
The science of photometry is the measurement of the changes in flux of objects, and it's a crucial component of researching variable stars.
Differential Photometry
Differential Photometry is comparing the difference between a target star and a comparison star, and eliminates all other observational variables.
Landolt
The Landolt catalog has become the de facto standard for transforming to the UBVR CIC system, and place photometric observations on a common platform.
Standard Photometric Stars
Photometric-standard stars are stars that have had their light output in various passbands of photometric system measured very carefully. They provide a means to not only calibrate your photometric system, but give a common “yardstick” from which all measurements can be compared.
Extinction
Extinction is the removal of light through dust, gas, or atmosphere, or the overall dimming of starlight by interstellar matter. Extinction comes in two types: Interstellar and Atmospheric.