mass ratio of 0.49, which has an uncertainty of about 10%. The mass ratio from the differential luminosity is 0.58, with a much larger (20%) uncertainty . Using the spectroscopic result, the primary (GJ 704A) has a mass of 0.94$M_\odot$, while the secondary (GJ 704B) is 0.46$M_\odot$.

The system configuration is shown in Figure \[fig:sys\] and is inclined such that the primary is currently closer to Earth than the secondary. The position of the B component relative to A on the date it was observed by *Herschel* in late April 2010 was PA=314$^\circ$ at an observed separation of 1.15” (22.6AU when deprojected), indicated by grey circles in the Figure.

A Third Component? {#s:third}
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While the STIS images clearly resolve the binary, there is a possible third component with $PA \approx 284^\circ$ and $\rho \approx 0.27"$ that is about 2.4 times as faint as the B component. @2008AN....329...54S also report a third component (epoch 2005.8) at $PA \approx 50^\circ$ and $\rho \approx 0.228"$ (no magnitude is given). However, while they detected the secondary again in mid-2007, they do not report any detection of the putative tertiary [@2010AN....331..286S]. The detected positions are shown as star symbols in sky coordinates in Figure 