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To understand the evolution of dust properties in molecular clouds in thecourse of the star formation process, we constrain the changes in the dustemissivity index from star-forming filaments to prestellar and protostellarcores to T Tauri stars. Using the NIKA2 continuum camera on the IRAM 30~mtelescope, we observed the Taurus B211/B213 filament at 1.2\,mm and 2\,mm withunprecedented sensitivity and used the resulting maps to derive the dustemissivity index $\beta$. Our sample of 105 objects detected in the $\beta$ mapof the B211/B213 filament indicates that, overall, $\beta$ decreases fromfilament and prestellar cores ($\beta \sim 2\pm0.5$) to protostellar cores($\beta \sim 1.2 \pm 0.2$) to T-Tauri protoplanetary disk ($\beta < 1$). Theaveraged dust emissivity index $\beta$ across the B211/B213 filament exhibits aflat ($\beta \sim 2\pm0.3$) profile. This may imply that dust grain sizes arerather homogeneous in the filament, start to grow significantly in size onlyafter the onset of the gravitational contraction/collapse of prestellar coresto protostars, reaching big sizes in T Tauri protoplanetary disks. Thisevolution from the parent filament to T-Tauri disks happens on a timescale ofabout 1-2~Myr.

NIKA2 observations of dust grain evolution from star-forming filament to  T-Tauri disk: Preliminary results from NIKA2 observations of the Taurus  B211/B213 filament