provided the first direct measurements of the wind speed on a brown dwarf, finding a strong eastward wind of $\sim650$m/s for the cool T dwarf 2MASS J10475385+2124234 [@Allers2020].]{} For the majority of directly-imaged planets however, the contrast between host star and planet make it difficult to obtain sufficiently high S/N photometry to allow precise variability monitoring [@Apai2016]. Young, free-floating brown dwarfs provide an excellent analog to directly-imaged planets. They share remarkably similar masses, radii and spectra with the directly-imaged planets [@Faherty2016; @Liu2013; @Liu2016] and can be observed in detail with current facilities.

In recent years variability studies of the low-gravity exoplanet analogs have revealed important insights into their atmospheres. @Metchev2015a noted a tentative correlation between low-gravity and high-amplitude variability in a sample of six mid-L type brown dwarfs as part of a larger *Spitzer* variability survey. A number of high-amplitude variability detections have since been reported in free-floating planetary-mass objects [@Biller2015; @Lew2016; @Vos2018; @Schneider2018] and wide, low-gravity companions [@Zhou2016; @Zhou2019; @Zhou2020; @Bowler2020]. In @Vos2019 we carried out a large ground-based, $J$-band survey for variability in isolated low-mass brown dwarfs, finding a $30\%$ variability fraction among low-gravity L dwarfs, compared to $11\%$ for the higher gravity, field brown dwarf population surveyed 