variability. This table includes their infrared amplitudes, rotation periods, estimated ages and inclination angles. Figure \[fig:amplitudes\] shows the full sample of field brown dwarfs and young brown dwarfs with measured *Spitzer* variability amplitudes on a spectral type color diagram. The area of the symbol size is proportional to the observed variability amplitude. [Upper limits on the variability amplitudes of brown dwarfs are shown by lighter colored circles with a cross. ]{}With the addition of and at early L spectral types we can begin to study the variability properties of the low-gravity population across the entire L sequence. While the sample is still relatively small some tentative trends emerge.

The left panel of Figure \[fig:amplitudes\_plot\] shows the measured $3.6~\mu$m variability amplitudes as a function of spectral type. It is apparent that the maximum amplitudes for both field and young dwarfs increase with cooler spectral type in the L sequence, as noted by @Metchev2015a for the field dwarf population. @Metchev2015a also find a tentative correlation between low-gravity and high-amplitude variability for the low-gravity objects with spectral types L3-L5.5. However, the current sample of low-gravity variables show similar $3.6~\mu$m amplitudes to the field dwarf population. It is worth noting that for each spectral 