3/19/21

 IC 348 is a compact young cluster located within the Perseus darkcloud complex at its eastern end; a detailed review of the cluster’sphysical properties and the studies done it was presented in the StarFormation Handbook by Herbst (2008).

3/18/21

 We also note what fraction of brown dwarfs do not match to objects in our catalog, comment upon the quality of the photometry of the given matches (especially if any brown dwarfs have problematic photometry unsuitable for further analysis), and describe any other issues (e.g., non-matches where a match was expected given previous photometric measurements).

3/17/21

 In this study, we have used catalogs of previously identified browndwarfs. This section summarizes the catalogs used in each region.

3/16/21

 Stars with high-quality photometry (high signal-to-noise, no dataprocessing flags, etc.), and high values of the Stetson variabilityindex for two or three bands, are selected as variable automatically.

3/15/21

 We made use of the analyticFAP estimation method described by Baluev (2008), as implementedwithin the AstroPy Lomb-Scargle package.

3/12/21

 The most common spacing between observations is approximately1 day, but the observations are irregularly sampled and not on a fixed24 hour period, so the true “Nyquist frequency” of these observationsis much higher than it would be if observations were sampled on afixed 24 hour grid (VanderPlas 2018); thus, it is statistically justifiableand scientifically worthwhile to choose a higher maximum frequency(lower minimum period) for our periodogram

3/11/21

We make use of the As-troPy (Astropy Collaboration et al. 2013, 2018) implementation ofthe Lomb-Scargle periodogram, based on the algorithms and imple-mentation described by VanderPlas et al. (2012) and VanderPlas &Ivezić (2015).