Counts

The video lesson assumes you have already reviewed the “Photometry an Overview”, “Comparison Stars”, and “Aperture Photometry” lessons. In this project, we’ll discuss the basic outline of a Photometry project from start to finish in order to put a global context to...

One of the capabilities of Photometry is to calculate magnitude of a given object. This is accomplished through Aperture Photometry. It is recommended that you have a good understanding of Aperture Photometry. Please review that lesson, if needed, before continuing.

The AAVSO Photometric All-Sky Survey (APASS) performed an allsky photometric survey in five filters: Johnson B and V, plus Sloan g′, r′, i′. The magnitudes range from 7th magnitude to about 17th magnitude. This catalog helps various research programs establish...

PSF stands for Point Spread Function which describes how an imaging system (ex. Telescope and CCD camera) image a singular point source such as a star. When a CCD image the object is divided into discrete point objects of varying intensity, each object is computed as...

When measuring the Flux (light) output of a star, there are a few methods to accomplish this. Two most common are: Aperture Photometry and Point Spread Function (PSF). This will focus on Aperture Photometry as it is the most accurate flux measurement, for non-crowded...

The science of Photometry is the measurement of changes in Flux (light) from an object, or objects, to better understand the nature of what you’re observing. This could be a variable star, eclipsing binary star, Exoplanet, quasar, supernova, novae, blazar, or any...