steeper slope from 1.1-1.25 $\mu$m and a wider peak at 1.30$\mu$m that is more similar to the field object. In a forthcoming paper, we will present a detailed $J$ band spectral analysis of 2M0355 and other young brown dwarfs compared to their field counterparts.

Several near-infrared spectral features are sensitive to surface gravity, including the $H$-band where a sharp triangular peak is seen consistently for known young brown dwarfs at a range of ages (e.g. @Lucas01; @Luhman04; @Allers07; @Rice10 [@Rice11]). In Figure \[fig:SpeX\], we present higher-resolution ($R\sim$1200) $H$-band spectra of 2M0355 as well as the same comparative objects shown in Figure \[fig:SpeX2\]. There is an excellent match between the sharp peak of 2M1207b and 2M0355, distinct from the plateau at $\sim$1.55–1.70 $\mu$m of the field object. Combined with the photometric peculiarities, this is a strong indicator that 2M0355 is significantly younger than the field object ($<<$ 1 Gyr).

Kinematics\[kinematics\]
------------------------

Using multi-epoch ISPI data (see Figure  \[fig:astrometry\]), we report improved proper motion and parallax measurements for 2M0355. The proper motion was measured previously by @Schmidt07, [@Casewell08], and [@Faherty09]. Our updated value is consistent with previous values but with 50-60$\%$ smaller error bars. The new parallax measurement of $\pi_{abs}$=122$\pm$13 mas[^4] for 