Eric E. Mamajek, Alejandro Núñez'
bibliography:
- 'paper2.bib'
title: '2MASSJ035523.37+113343.7: A Young, Dusty, Nearby, Isolated Brown Dwarf Resembling A Giant Exoplanet'
---

2MASSJ035523.37+113343.7

INTRODUCTION
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With masses intermediate between stars and planets (i.e., below the hydrogen burning and above the deuterium burning mass limit), brown dwarfs provide a natural link between stellar astrophysics and the planetary science of gas-giants (@Saumon1996; @Chabrier1997). Studies of the population have informed our understanding of low-mass star formation as well as the physical and chemical composition of low-temperature photospheres (e.g. @Burrows01 [@Burrows97]; @Chabrier00). With an increasing number of brown dwarf discoveries, the diversity of the population in age, atmospheric properties, and chemical composition is becoming apparent.

Brown dwarfs are classified using red optical or near-infrared spectra and show characteristics which distinguish them as L (T$_{eff}\sim$2200 - 1300K) or T/Y (T$_{eff}<$1300) dwarfs (@Kirkpatrick99; @Burgasser02; @Cushing11). The majority of spectrally classified field brown dwarfs within the literature are nearby isolated L dwarfs. Among the $\sim$1000 objects spanning this temperature regime, a significant portion exhibit near-infrared colors, spectral energy distributions (SEDs), and kinematics consistent with a field age population (e.g., @Kirkpatrick00; @Knapp04; @Cruz07; @Chiu06; @Faherty09; @Schmidt10). However there are subsets exhibiting strong deviations in observational properties from the 