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We examined the grain size in the dust ring encircling the 0.19~$M_\sun$ TTauri star CIDA 1 using the Karl G. Jansky Very Large Array (JVLA) at multiplecentimeter wavelengths, with a spatial resolution of 0$\farcs$2--0$\farcs$9. Wedetected distinct partial-ring structures at these wavelengths around CIDA~1.Based on spatial distributions and spectral indexes, we determined that thesecentimeter emissions originated from dust, rather than free-free or synchrotronemissions. To estimate the maximum grain size ($a_{\rm max}$) within the ring,we compared the observed spectral energy distribution (SED) with SEDscalculated for different $a_{\rm max}$ values using radiative transfercalculations. Our findings indicate an $a_{\rm max}$ value of approximately2.5~cm in the ring, assuming the dust opacity can be approximated by the DSHARPmodels. These results suggest that grain growth took place within the CIDA~1ring, potentially facilitating more efficient planet formation through pebbleaccretion scenarios involving centimeter-sized pebbles.

Centimeter-sized Grains in the Compact Dust Ring around Very Low Mass Star CIDA 1