On the face of it, the long term V, R and I data of 2MASS 20512895+4404230 (1st image) looks ordinary and boring. No visible change, just a bit of noise. The star is just over one arcminute away from the much more exciting old friend of the project V2492Cyg. According to Gaia, our data for 2MASS 20512895+4404230 actually consists of two stars, less than two arcseconds apart. They are hence unresolved in our images. However, the brighter star is about 4mag brighter than the other one. Thus, the light we detect is to 97.5% from the brighter star. Gaia also places it at the correct distance to be a member of the Pelican nebula young star population (d=791pc). Furthermore, photometry across all wavelengths indicates an (albeit weak) infrared access, indicating an accretion disk.
However, if one analyses our data and searches for periodic behaviour, a clear period of 4.826days is found. The amplitude of the variability at all wavelengths is rather large, reaching between 10 and 15% of the flux. Indeed, if one zooms in to our data, this periodicity is even evident to the naked eye (2nd picture). We are currently working on detailed analysis of light curves like this to determine the properties of the surface spots causing these variations. I.e. we plan to determine the temperature and size of the spot. This is part of an ongoing PhD thesis, so expect more detailed discussions of results from this in the not too far future.