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An initial three-station version of the Event Horizon Telescope, amillimeter-wavelength very-long baseline interferometer, has observedSagittarius A* (Sgr A*) repeatedly from 2007 to 2013, resulting in themeasurement of a variety of interferometric quantities. Of particularimportance, there is now a large set of closure phases, measured over a numberof independent observing epochs. We analyze these observations within thecontext of a realization of semi-analytic radiatively inefficient disk models,implicated by the low luminosity of Sgr A*. We find a broad consistency amongthe various observing epochs and between different interferometric data types,with the latter providing significant support for this class of models of SgrA*. The new data significantly tighten existing constraints on the spinmagnitude and its orientation within this model context, finding a spinmagnitude of $a=0.10^{+0.30+0.56}_{-0.10-0.10}$, an inclination with respect tothe line of sight of$\theta={60^\circ}^{+5^\circ+10^\circ}_{-8^\circ-13^\circ}$, and a positionangle of $\xi={156^\circ}^{+10^\circ+14^\circ}_{-17^\circ-27^\circ}$ east ofnorth. These are in good agreement with previous analyses. Notably, theprevious $180^\circ$ degeneracy in the position angle has now been conclusivelybroken by the inclusion of the closure phase measurements. A reflectiondegeneracy in the inclination remains, permitting two localizations of the spinvector orientation, one of which is in agreement with the orbital angularmomentum of the infrared gas cloud G2 and the clockwise disk of young stars.This possibly supports a relationship between Sgr A*'s accretion flow and theselarger-scale features.

Modeling Seven Years of Event Horizon Telescope Observations with Radiatively Inefficient Accretion Flow Models