resolved, making the true dust location uncertain. Resolved systems such as 99 Her remove this ambiguity, and provide crucial information on the disk location, stability and dynamics.

This paper is laid out as follows. We first consider the stellar and orbital properties of the 99 Her system, including the possibility of a third component. Then we consider the *Herschel* image data and several different models that can explain it. Finally, we discuss the implications of these models for the formation of the system.

99 Herculis {#s:stprop}
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The binary 99 Herculis (HD 165908, HIP 88745, GJ 704AB, ADS 11077) contains the 37$^{\rm
  th}$ closest F star primary within the volume limited Unbiased Nearby Stars sample [@2010MNRAS.403.1089P]. The Catalogue of Components of Doubles and Multiple systems [CCDM J18071+3034, @2002yCat.1274....0D] lists three components, but using Hipparcos proper motions @2010MNRAS.403.1089P find that the 93” distant C component is not bound to the system. The binary pair has been known since 1859, and consists of an F7V primary orbited by a K4V secondary. The primary is known to be metal poor with \[Fe/H\] $\approx -0.4$ [e.g. @1996yCat..33140191G; @2000MNRAS.316..514A; @2007PASJ...59..335T] and has an age consistent with the main-sequence .

Binary Configuration {#ss:binary}
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  Parameter                    Symbol 