The Envelope Kinematics and a Possible Disk Around the Class 0 Protostar
  within BHR7
  We present a characterization of the protostar embedded within the BHR7 dark
cloud, based on both photometric measurements from the near-infrared to
millimeter and interferometric continuum and molecular line observations at
millimeter wavelengths. We find that this protostar is a Class 0 system, the
youngest class of protostars, measuring its bolometric temperature to be
50.5~K, with a bolometric luminosity of 9.3~L$_{\odot}$. The near-infrared and
\textit{Spitzer} imaging show a prominent dark lane from dust extinction
separating clear bipolar outflow cavities. Observations of $^{13}$CO
($J=2\rightarrow1$), C$^{18}$O ($J=2\rightarrow1$), and other molecular lines
with the Submillimeter Array (SMA) exhibit a clear rotation signature on scales
$<$1300~AU. The rotation can be traced to an inner radius of $\sim$170~AU and
the rotation curve is consistent with an R$^{-1}$ profile, implying that
angular momentum is being conserved. Observations of the 1.3~mm dust continuum
with the SMA reveal a resolved continuum source, extended in the direction of
the dark lane, orthogonal to the outflow. The deconvolved size of the continuum
indicates a radius of $\sim$100~AU for the continuum source at the assumed
distance of 400~pc. The visibility amplitude profile of the continuum emission
cannot be reproduced by an envelope alone and needs a compact component. Thus,
we posit that the resolved continuum source could be tracing a Keplerian disk
in this very young system. If we assume that the continuum radius traces a
Keplerian disk (R$\sim$120~AU) the observed rotation profile is consistent with
a protostar mass of 1.0~$M_{\odot}$.
