Epsilon Indi

Yiting Li, incontent with rewriting all we thought we knew about nearby gas-giants, has carried on to the best brown-dwarf twin: Epsilon Indi B.

The DR3, joined with this systems' massive parallax (3.638 parsecs!), and the two decades we've had since B was found to be a BC itself, have all allowed Li and Chen and the rest to constrain masses for the B and the C ("Bb" in this paper): about 66 M_j and 53.25 M_j both T-class although the larger one is almost L. The dataset 2005-16 covers the eleven years the pair take to orbit their barycentre.

It is found that the big one is much more luminous than the "small" one after the 3.5 Gy proterozoic age of A. The larger one might not be burning deuterium for much longer. Possibly why it took until 2004 even to know that BC was a binary.

This hints that T dwarfs will be difficult to spot against the brighter stars if those systems are further from us; especially if they roll closer to those stars and/or are sub-50 in mass.

This also suggests Philipot to revise his team's priors, for A. BC together is not Dieterich et al. 2018's total 145 M_j; it is 120 M_j. At 1460 AU between A and BC, this might reduce the error-bars for Aa.