Alma Survey Of Circumstellar Disks In The Young Stellar Cluster IC 348
  We present a 1.3 mm continuum survey of the young (2-3 Myr) stellar cluster
IC 348, which lies at a distance of 310 pc, and is dominated by low-mass stars
(M$_{\star}$ $\sim$ 0.1-0.6 M$_{\odot}$). We observed 136 Class II sources
(disks that are optically thick in the infrared) at 0.8$''$ (200 au) resolution
with a 3$\sigma$ sensitivity of $\sim$ 0.45 mJy (M$_{\rm dust}$ $\sim$ 1.3
M$_{\oplus}$). We detect 40 of the targets and construct a mm-continuum
luminosity function. We compare the disk mass distribution in IC 348 to those
of younger and older regions, taking into account the dependence on stellar
mass. We find a clear evolution in disk masses from 1 to 5-10 Myr. The disk
masses in IC 348 are significantly lower than those in Taurus (1-3 Myr) and
Lupus (1-3 Myr), similar to those of Chamaleon~I, (2-3 Myr) and $\sigma$ Ori
(3-5 Myr) and significantly higher than in Upper Scorpius (5$-$10 Myr). About
20 disks in our sample ($\sim$5$\%$ of the cluster members) have estimated
masses (dust $+$ gas) $>$1 M$_{\rm Jup}$ and hence might be the precursors of
giant planets in the cluster. Some of the most massive disks include transition
objects with inner opacity holes based on their infrared SEDs. From a stacking
analysis of the 96 non-detections, we find that these disks have a typical dust
mass of just $\lesssim$ 0.4 M$_{\oplus}$, even though the vast majority of
their infrared SEDs remain optically thick and show little signs of evolution.
Such low-mass disks may be the precursors of the small rocky planets found by
\emph{Kepler} around M-type stars.
