This project is intended to encourage observers to check their accuracy and repeatability of observations, using some known Landolt Fields, that have been well observed by Arne Henden (He has actually observed these more than Landolt did). This project will allow observers to check methodologies--ie SN, Flatfielding, Dark Subtraction, Software Reductions, etc.

What you do is perform a time series (of 15-20 multiple exposures) of a Standard Field, which is well known. Thanks to Bruce Gary and Arne Henden, we have selected 13 of these fields, which means that one should be up at the meridian nearly every night. A table with the names and the magnitudes can be found on the AAVSO website.

Observe a field in V filtered, untransformed. Reduce each exposure separately. Do not average your exposures. Measure Star A relative to Star B only. Each exposure should be according to your normal procedure - a good rule of thumb is to expose long enough for the brightest star in the process to register half of full well. Report your results to HQ using WebObs or your standard procedure, that way we can share the light "curves" with all observers. Use the star name and letter A (ie SA114A) listed in the web page above for your v instrumental magnitudes (V filtered by untransformed).