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The formation scenario of brown dwarfs is still unclear because observationalstudies to investigate its initial condition are quite limited. Our systematicsurvey of nearby low-mass star-forming regions using the Atacama Compact Array(aka Morita array) and the IRAM 30 m telescope in 1.2 mm continuum hasidentified a centrally concentrated starless condensation with a central H$_2$volume density of $\sim$10$^6$ cm$^{-3}$, MC5-N, connected to a narrow (width$\sim$0.03 pc) filamentary cloud in the Taurus L1495 region. The mass of thecore is $\sim$0.2-0.4 $M_{\odot}$, which is an order of magnitude smaller thantypical low-mass prestellar cores. Taking into account a typical core to starformation efficiency for prestellar cores ($\sim$20%-40%) in nearby molecularclouds, brown dwarf(s) or very low-mass star(s) may be going to be formed inthis core. We have found possible substructures at the high-density portion ofthe core, although much higher angular resolution observation is needed toclearly confirm them. The subsequent N$_2$H$^+$ and N$_2$D$^+$ observationsusing the Nobeyama 45 m telescope have confirmed the high-deuteriumfractionation ($\sim$30%). These dynamically and chemically evolved featuresindicate that this core is on the verge of proto-brown dwarf or very low-massstar formation and is an ideal source to investigate the initial conditions ofsuch low-mass objects via gravitational collapse and/or fragmentation of thefilamentary cloud complex.

A centrally concentrated sub-solar mass starless core in the Taurus L1495 filamentary complex