  The earliest stages of low-mass star-formation are unclear, but it has been
proposed that Chamaeleon-MMS1 is a candidate First Hydrostatic Core (FHSC), the
transition stage between a prestellar and protostellar core. This work
describes the local (~4000 AU) outflow activity associated with Chamaeleon-MMS1
and its effect on the surrounding material in order to determine the
evolutionary state of this young low-mass source. We used the Atacama Large
Millimeter/sub-millimeter Array (ALMA) to observe Chamaeleon MMS1 at 220 GHz at
high spatial (~75 AU) and spectral resolutions (0.1-0.3 km/s). A low energy
outflow is detected through its interaction with the surrounding cloud. The
outflow consists of two components, a broad spectral feature to the northeast
and narrow features to both the northeast and southwest. The rotational
temperature of formaldehyde (H2CO) is calculated to be 50 (+/-30) K toward the
continuum source with similarly low temperatures (25-45 K) toward clumps
affected by the outflow. Methanol (CH3OH) is only detected toward gas clumps
located away from the continuum source, where the methanol is expected to have
been released by the energy of the outflow through ice sputtering in shock
waves. Chamaeleon-MMS1 shows outflow activity with the power source being
either a single precessing outflow or two outflows from a binary system. While
molecular emission and high outflow speeds rule it out as a FHSC, the outflow
is less energetic than outflows detected from other Class 0 objects and the
inferred gas temperatures toward the continuum source are relatively low, which
indicates that Cha-MMS1 is one of the youngest known sources.
