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tokens: of a desert beyond. However, of the 382 stars in their sample, only 36 are solar-type (main-sequence with 5000 T eff 6000K) stars. Troup etal. ( 2016 ) argue that this result agrees with the work of Guillot etal. ( 2014 ) who find that the BD desert may not be as dry as initially thought when considering stars more massive than the Sun, as well as evidence that the BD desert is a special case for solar-mass stars (Duchne Kraus 2013 ). Duchne Kraus ( 2013 ) suggest tidal interaction with host stars may shape the brown dwarf desert. While assessing the characteristic time-scale for orbital decay, Damiani Daz ( 2016 ) find that F-type stars may host massive companions for a significantly longer time than G-type stars for orbital periods less than 5 d; however, they conclude that BD occurrence should largely be unaffected by tidal decay for orbital periods greater than 10 d, regardless of host mass. Debate continues on valid formation mechanisms of BDs and whether or not different formation mechanisms dominate in different mass, period and eccentricity regimes. Three main mechanisms are advocated in the field: (i) the ejection of protostellar embryos from their natal cloud cores (Boss 2001 ; Reipurth Clarke 2001 ), (ii) the fragmentation of protostellar discs (Stamatellos Whitworth 2009 ; Stamatellos etal. 2011 ) or (iii) collapsing molecular cloud cores (Hopkins 2012 ; Hennebelle Chabrier 2013 ), i.e. the same process as Sun-like stars. Through their statistical study, Ma Ge ( 2014 ) reported that BD companions with minimum masses below 42.5 M Jup have an eccentricity distribution consistent with that of massive planets, while those with masses above 42.5 M Jup have an eccentricity distribution consistent with that of binaries. Ma Ge ( 2014 ) also find that host stars of BD companions are not metal rich and have a significantly different metallicity distribution compared to host stars of giant planets, suggesting a formation mechanism different from the core-accretion (Ida Lin 2004 ) scenario. Ma Ge ( 2014 ) conclude that BD companions with minimum masses below 42.5 M Jup likely form in a protoplanetary disc through the disc gravitational instability scenario, and their eccentricity is excited through scattering, while BD companions with minimum masses above 42.5 M Jup likely form in the same way as stars, through molecular cloud fragmentation. Troup etal. ( 2016 ) find 14 candidate BD companions around metal-poor stars ([Fe/H]0.5), also challenging the core-accretion formation model for BDs, which they find unsurprising given that Carney etal. ( 2003 ) observed that lower metallicity populations generally have a higher number of binaries. Here, we present new BD candidate companions using data from the SDSS-III Multi-object APO Radial Velocity Exoplanet Large-area Survey (MARVELS; Ge etal. 2008 ). MARVELS observed 3300 stars with 10 RV measurements. Unlike APOGEE, MARVELS primarily targeted solar-like dwarfs, and thus, is complementary to the