The young variable star V1492Cyg is situated in the Pelican Nebula (IC5070) Target region of HOYS. It is a member of the young cluster and known by a number of other names. One of them, LkHa149 also identifies it as an emission line source, i.e. an actively accreting object. Indeed it shows excess emission in the Hydrogen alpha observations in our dataset.
In the above image we show about 250 days worth of V and I-band data for the source from the summer of 2024. There are number of outliers visible in the V-band data, which our calibration and ‘cleaning’ process will remove before any detailed analysis. But we can see the main behaviour of the source. There is some general stochastic variability of up to a few 10 percent. In addition there is a 2-3 week long dimming event of one magnitude at the start of the data.
These sort of events are hinting at denser, small scale structures, usually in the inner disk. One of the things we are working on is the statistics of these events. How often do they occur? How long are they? How deep are they? Comparing these to models will allow us ultimately to put constraints on the small scale structures (percent AU scales) in the inner disks around young stars.