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Young brown dwarfs are analogs to giant exoplanets, as they share effectivetemperatures, near-infrared colors, and surface gravities. Thus, the detailedcharacterization of young brown dwarfs might shed light on the study of giantexoplanets, that we are currently unable to observe with sufficientsignal-to-noise to allow precise characterization of their atmospheres. 2MASSJ22081363+2921215 is a young L3 brown dwarf, member of the beta-Pictoris youngmoving group (23 +/-3 Myr), that shares its effective temperature and mass withthe beta Pictoris b giant exoplanet. We performed a ~2.5 hr spectro-photometricJ-band monitoring of 2MASS J22081363+2921215 with the MOSFIRE multi-objectspectrograph, installed at the Keck I telescope. We measured a minimumvariability amplitude of 3.22 +/- 0.42 % for its J-band light curve. The ratiobetween the maximum and the minimum flux spectra of 2MASS J22081363+2921215shows a weak wavelength dependence and a potential enhanced variabilityamplitude in the alkali lines. Further analysis suggests that the variabilityamplitude on the alkali lines is higher than the overall variability amplitude(4.5-11 %, depending on the lines). The variability amplitudes in these linesare lower if we degrade the resolution of the original MOSFIRE spectra toR~100, which explains why this potential enhanced variability in the alkalilines has not been found previously in HST/WFC3 light curves. Usingradiative-transfer models, we obtained the different cloud layers that might beintroducing the spectro-photometric variability we observe for 2MASSJ22081363+2921215, that further support the measured enhanced variabilityamplitude in the alkali lines. We provide an artistic recreation of thevertical cloud structure of this beta-Pictoris b analog.

the astronomical journal

Revealing the Vertical Cloud Structure of a young low-mass Brown Dwarf,  an analog to the beta-Pictoris b directly-imaged exoplanet, through Keck  I/MOSFIRE spectro-photometric variability