Investigating Molecular Gas Properties of Class 0 Source CARMA-7

Previous observations of the low mass Class 0 protostar, CARMA-7, in the Serpens South cluster region detected outflow ejection events traced by $^{12}CO$ J=2→1. However, little is known about the molecular abundances and morphologies of molecular lines other than carbon monoxide isotopologues. We present follow-up observations of 9 molecular emission lines near CARMA-7 using the Atacama Large Millimeter/sub-millimeter Array. We confirm the presence of a bipolar outflow extending in the north-south direction with a position angle of 4$^{\circ}$ as traced by $^{12}CO$ J=2→1, $H_{2}CO$ 3(0,3)-2(0,2), and $H_{2}CO$ 3(2,1)-2(2,0). Further investigation of the $H_{2}CO$ and $c-C_{3}H_{2}$ lines uncovered a low velocity extended emission feature slanted to the southwest with a position angle of 72$^{\circ}$. We interpret this feature as a potential accretion flow, but further analysis via modeling is necessary. The $C^{18}O$ 2→1 emission line shows early signs of Keplerian rotation in the disk/envelope. However, other known disk and envelope tracers such as $^{13}CO$, $N_{2}D^{+}$, and $H_{2}CO$ fail to show signs of rotation. We find that CARMA-7 does not hold a disk larger than 305 AU and that the detection of a strong outflow is not a clear indicator of an evolved disk.