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We present a survey of 28 molecular outflows driven by low-mass protostars,all of which are sufficiently isolated spatially and/or kinematically to fullyseparate into individual outflows. Using a combination of new and archival datafrom several single-dish telescopes, 17 outflows are mapped in CO (2-1) and 17are mapped in CO (3-2), with 6 mapped in both transitions. For each outflow, wecalculate and tabulate the mass, momentum, kinetic energy, mechanicalluminosity, and force assuming optically thin emission in LTE at an excitationtemperature of 50 K. We show that all of the calculated properties areunderestimated when calculated under these assumptions. Taken together, theeffects of opacity, outflow emission at low velocities confused with ambientcloud emission, and emission below the sensitivities of the observationsincrease outflow masses and dynamical properties by an order of magnitude, onaverage, and factors of 50-90 in the most extreme cases. Different (andnon-uniform) excitation temperatures, inclination effects, and dissociation ofmolecular gas will all work to further increase outflow properties. Molecularoutflows are thus almost certainly more massive and energetic than commonlyreported. Additionally, outflow properties are lower, on average, by almost anorder of magnitude when calculated from the CO (3-2) maps compared to the CO(2-1) maps, even after accounting for different opacities, map sensitivities,and possible excitation temperature variations. It has recently been argued inthe literature that the CO (3-2) line is subthermally excited in outflows, andour results support this finding.

Molecular Outflows Driven by Low-Mass Protostars. I. Correcting for Underestimates When Measuring Outflow Masses and Dynamical Properties