discussed until @Reid08 and @Cruz09. 2M0355 is classified as an L5$\gamma$ dwarf[^2], demonstrating strong Li absorption (EW 7.0$\AA$) and other signatures of low surface gravity in the optical (@Reid08, @Cruz09). Notably this source is the reddest isolated L dwarf yet classified, with a 2MASS $J-K_{s}$ color of 2.52$\pm$0.03.

@Reid06 examined 2M0355 for a close companion with the Near-Infrared Camera and Mutli-Object Spectrometer NIC1 on the *Hubble Space Telescope* and found it unresolved. @Blake07 examined this source for radial velocity variations but found no appreciable change over time and excluded the possibility of a companion with $M$ $sin$ $i$ $>$ 2.0 M$_{J}$ at any separation. We note that @Blake07 assumed an L dwarf primary mass of 100 M$_{J}$ which is large for even a field aged object, therefore, given the RV constraints, the limit is likely below 2.0 M$_{Jup}$. @Bernat10 claimed the detection of a near-equal mass companion at 82.5 mas using aperture masking interferometry; however, this result falls at the low end of their confidence limits (90%) and such a companion should have been detected by the @Reid06 imaging campaign (although @Bernat10 note this object may be at the limit of @Reid06 detections).

Radial velocities of 12.24$\pm$0.18 and 11.92$\pm$0.22 km 