The Spitzer c2d Survey Of Nearby Dense Cores. IX. Discovery Of A Very Low Luminosity Object Driving A Molecular Outflow In The Dense Core L673-7

We present new infrared, submillimeter, and millimeter observations of the dense core L673-7 and report the discovery of a low-luminosity, embedded Class 0 protostar driving a molecular outflow. L673-7 is seen in absorption against the mid-infrared background in 5.8, 8, and 24 mu m Spitzer images, allowing for a derivation of the column density profile and total enclosed mass of L673-7, independent of dust temperature assumptions. Estimates of the core mass from these absorption profiles range from 0.2 to 4.5M(circle dot). Millimeter continuum emission indicates a mass of similar to 2M(circle dot), both from a direct calculation assuming isothermal dust and from dust radiative transfer models constrained by the millimeter observations. We use dust radiative transfer models to constrain the internal luminosity of L673-7, defined to be the luminosity of the central source and excluding the luminosity from external heating, to be L(int) = 0.01-0.045L(circle dot), with L(int) similar to 0.04L(circle dot) the most likely value. L673-7 is thus classified as a very low luminosity object (VeLLO), and is among the lowest luminosity VeLLOs yet studied. We calculate the kinematic and dynamic properties of the molecular outflow in the standard manner. From the outflow properties and standard assumptions regarding the driving of outflows, we calculate the time-averaged protostellar mass accretion rate, total protostellar mass accreted, and expected accretion luminosity to be >= 1.2 x 10(-6) sin i/cos(2) i M(circle dot) yr(-1), M(acc) >= 0.07 1/cos i M(circle dot), and L(acc) >= 0.36L(circle dot), respectively. The discrepancy between this calculated L(acc) and the L(int) derived from dust radiative transfer models indicates that the current accretion rate is much lower than the average rate over the lifetime of the outflow. Although the protostar embedded within L673-7 is consistent with currently being substellar, it is unlikely to remain as such given the substantial mass reservoir remaining in the core.NASA 1224608, 1288664, 1288658, RSA 1377304, NNX 07-AJ72G, 1279198, 1288806NSF AST-0607793UT Austin UniversityAstronom