SMA 200-400 GHz Survey for Dust Properties in the Icy Class II Disks in the Taurus Molecular Cloud
We present a new SMA survey of 47 Class II sources in the Taurus-Auriga region. Our observations made 12 independent samples of flux densities over the 200-400 GHz frequency range. We tightly constrained the spectral indices of most sources to a narrow range of $2.0\pm0.2$; only a handful of spatially resolved (e.g., diameter $>$250 au) disks present larger spectral indices. The simplest interpretation for this result is that the (sub)millimeter luminosities of all of the observed target sources are dominated by very optically thick (e.g., $τ\gtrsim$5) dust thermal emission. Some previous works that were based on the optically thin assumption thus might have underestimated optical depths by at least one order of magnitude. Assuming DSHARP dust opacities, this corresponds to underestimates of dust masses by a similar factor. Moreover, some population synthesis models show that to explain the observed, narrowly distributed spectral indices, the disks in our selected sample need to have very similar dust temperatures ($T_{\small{dust}}$). Given a specific assumption of median $T_{\small{dust}}$, the maximum grain sizes ($a_{\small{max}}$) can also be constrained, which is a few times smaller than 0.1 mm for $T_{\small{dust}}\sim$100 K and a few mm for $T_{\small{dust}}\sim$24 K. The results may indicate that dust grain growth outside the water snowline is limited by the bouncing/fragmentation barriers. In the Class II disks, the dust mass budget outside of the water snowline may be largely retained instead of being mostly consumed by planet formation. While Class II disks still possess sufficient dust masses to feed planet formation at a later time, it is unknown whether or not dust coagulation and planet formation can be efficient or natural outside of the water snowline.