3/31/21

  ASpitzerinfrared survey ofIC 348 was presented by Muench et al. (2007), identifying this asa cluster with approximately 420 members, of which 118 are ClassII disked members and 31 are (Class 0 or I) protostars.

3/30/21

 The age of NGC 1333 has been estimated in the1−2Myr rangeby Bally et al. (2008); Walawender et al. (2008); Gutermuth et al.(2008).

3/29/21

 The age of IC 348 was estimated in the 2-6 Myr range (luhman2003, bell 2013), with 3 Myr taken as a representative age by Luhmanet al. 2020.

3/26/21

 Kounkel et al. (2018) present a distance to the ONC of 386±3 pcusing an analysis of APOGEE,Gaia, and VLBA data

3/25/21

 In these studies, Rebull et al. have discovered that, withsensitive enough photometric monitoring, nearly all stars displayperiodic photometric variability.

3/24/21

  The optical variabilityof young (∼1−10Myr) low-mass stars was studied by Rebullet al. (2018, 2020) using theKeplerK2 mission, with high-cadence,high-precision single-band photometry.

3/23/21

  Ortiz-León et al. (2018) derive a distanceof321±10pc for IC 348, based on a combined analysis of VLBA andGaiaastrometry. Zucker et al. (2018) report a distance of295±14pcto IC 348, based on a joint Bayesian analysis of Pan-STARRS and2MASS photometry, CO kinematics, andGaiaastrometry. [

3/22/21

 NGC 1333– The star cluster NGC 1333, and its nearby compan-ion IC 348 (discussed below), are both part of the broader Perseusmolecular cloud (properties summarized by Bally et al. 2008), a star-forming molecular cloud with about104푀lying at approximately300 pc distance.

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).