A broader Planet-Brown Dwarf Upper Limit?

Statistical Properties of Brown Dwarf Companions: Implications for Different Formation Mechanisms

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Analysis conducted in this paper was also able to provide a clue about this upper mass limit. The cumulative BD mass distribution (Fig. 3) suggests this limit is in the range 30−60 M_Jup and mass-eccentricity relation (Fig. 5) suggests that this limit is around 43 M_Jup. It appears that the upper limit is around 43 M_Jup, which is consistent with the result found by Grether & Lineweaver (2006), but is slightly larger than that from Sahlmann et al. (2011b).

In this case the number of high-mass planetary objects would significantly rise (to say, I would include MARVELS-1 b, MARVELS-4 b and much more).

But the problem is the existence of isolated planetary bodies, likely formed as stars and not as planets. Very difficult to explain with ejection mechanisms.

My opinion is that exists a range of masses in which both type of formations overlap.

Would that be similar to main-sequence stars of similar mass but different spectral types?

Also, is the 43Mj the new upper limit for a planet?

-M-

So CoRoT-15 b may be a supermassive "planet"

Stalker wrote:

So CoRoT-15 b may be a supermassive "planet"

Not really. With 63.3 Jupiter masses it quite lies in brown dwarf regime.

But HD 168443 c and HD 106252 b (the latter with astrometric mass) could.

As well as a 35 Mj (minimum mass) circumbinary companion at 21 Herculis and MARVELS-1 b and MARVELS-4 Ab too.