Color weight photometry

Four-color and Hp Photometry of Stars

Flicker photometry with chromatic adaptation and defective color vision.

When we alternate red and green stimuli at a certain frequency, we observe a flicker­ ing field. By adjusting luminances of both stimuli, we can minimize the flicker percep­ tion. This is the principle of the flicker pho­ tometry. When we apply the method to color defects, both subjects who are protanomal and those who are protanopic show a defi­ nitely different adjustment of two lumi­ nances ...

Empirical Color Transformations Between SDSS Photometry and Other Photometric Systems

Aims. We present empirical color transformations between the Sloan Digital Sky Survey (SDSS) ugriz photometry and Johnson-Cousins UBVRI system and Becker’s RGU system, respectively. Owing to the magnitude of data that is becoming available in the SDSS photometric system it is particularly important to be able to convert between this new system and traditional photometric systems. Unlike earlier...

Using color photometry to separate transiting exoplanets from false positives

The radial velocity technique is currently used to classify transiting objects. While capable of identifying grazing binary eclipses, this technique cannot reliably identify blends, a chance overlap of a faint background eclipsing binary with an ordinary foreground star. Blends generally have no observable radial velocity shifts, as the foreground star is brighter by several magnitudes and ther...

Not Color Blind: Using Multiband Photometry to Classify Supernovae

Large numbers of supernovae (SNe) have been discovered in recent years, and many more will be found in the near future. Once discovered, further study of a SN and its possible use as an astronomical tool (e.g., as a distance estimator) require knowledge of the SN type. Current classification methods rely almost solely on the analysis of SN spectra to determine their type. However, spectroscopy ...