exoplanets on this color-magnitude diagram–which are also redward and underluminous of the brown dwarf population–can be reproduced by allowing low T$_{eff}$ models (typically assumed cloud-free) to have clouds extending across their photospheres (see also @Bowler10; @Currie11; @Hinz10; @Marley12; @Madhusudhan11; @Skemer12). 2M1207b and HR8799bcd are young ($\sim$10 Myr and 30-160 Myr; respectively: @Chauvin04; @Marois08; @Marois10) so youth is thought to be correlated with enhanced photospheric dust among the low-luminosity, low-temperature brown dwarfs and giant exoplanets (see also @Burgasser10; @Faherty12).

Consequently, the position of 2M0355 on Figure  \[fig:TM0355\] leads us to conclude that in agreement with indications from the SED in Figure  \[fig:SED\] this source is both young and dusty.

Conclusions
===========

2M0355 is the reddest isolated L dwarfs yet characterized in the near- and mid-infrared. @Cruz09 classified 2M0355 as L5$\gamma$, indicating low surface gravity spectral signatures. The similarity of the near-infrared spectrum to that of the $\sim$10 Myr planetary-mass object 2M1207b supports the conclusion that the object is young. Furthermore, a comparison with the near and mid-infrared colors of the known population of low surface gravity or L$\gamma$ dwarfs demonstrates that 2M0355 is the most extreme example of this class currently known.

Combining optical spectra and absolute near to mid-IR photometry, 