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The first hydrostatic core, the first quasi-hydrostatic object formed duringthe star formation process, is still the observational missing link between theprestellar and protostellar phases, mainly due to its short lifetime. Althoughwe have not established a clear method to identify this rare object, recenttheoretical studies predict that the first core has millimeter continuumemission and low-velocity outflow with a wide opening angle. An extensivecontinuum/outflow survey toward a large number of $"$starless$"$ cores innearby star-forming regions works as a pathfinder. We observed 32 prestellarcores in Taurus with an average density of $\gtrsim$10$^5$ cm$^{-3}$ in 1.3 mmcontinuum and molecular lines using the Atacama Large Millimeter/submillimeterArray$-$Atacama Compact Array (ALMA$-$ACA) stand-alone mode. Among the targets,MC35-mm centered at one of the densest $"$starless$"$ cores in Taurus hasblueshifted/redshifted wings in the $^{12}$CO (2-1) line, indicating that thereis deeply embedded object driving molecular outflow. The observed velocitiesand sizes of the possible outflow lobes are 2-4 km s$^{-1}$, and $\sim$2$\times$10$^3$ au, respectively, and the dynamical time is calculated to be$\sim$10$^3$ yr. In addition to this, the core is one of the strongestN$_2$D$^{+}$ (3-2) emitters in our sample. All of the observed signatures donot conflict with any of the theoretical predictions about the firsthydrostatic core so far, and thus MC35-mm is unique as the only first-corecandidate in the Taurus molecular cloud.

A low-velocity bipolar outflow from a deeply embedded object in Taurus revealed by the Atacama Compact Array