The Flux Distribution of Sgr A*
  The Galactic Center black hole Sagittarius A* is a variable NIR source that
exhibits bright flux excursions called flares. The low-flux density turnover of
the flux distribution is below the sensitivity of current single-aperture
telescopes. We use the unprecedented resolution of the GRAVITY instrument at
the VLTI. Our light curves are unconfused, overcoming the confusion limit of
previous photometric studies. We analyze the light curves using standard
statistical methods and obtain the flux distribution. We find that the flux
distribution of SgrA* turns over at a median flux density of (1.1\pm0.3)mJy. We
measure the percentiles of the flux distribution and use them to constrain the
NIR K-band SED. Furthermore, we find that the flux distribution is
intrinsically right-skewed to higher flux density in log space. Flux densities
below 0.1mJy are hardly ever observed. In consequence, a single powerlaw or
lognormal distribution does not suffice to describe the observed flux
distribution in its entirety. However, if one takes into account a power law
component at high flux densities, a lognormal distribution can describe the
lower end of the observed flux distribution. We confirm the RMS-flux relation
for Sgr~A* and find it to be linear for all flux densities in our observation.
We conclude that Sgr~A* has two states: the bulk of the emission is generated
in a lognormal process with a well-defined median flux density and this
quiescent emission is supplemented by sporadic flares that create the observed
power law extension of the flux distribution.
