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In recent years evidence has been building that planet formation startsearly, in the first $\sim$ 0.5 Myr. Studying the dust masses available in youngdisks enables understanding the origin of planetary systems since mature disksare lacking the solid material necessary to reproduce the observed exoplanetarysystems, especially the massive ones. We aim to determine if disks in theembedded stage of star formation contain enough dust to explain the solidcontent of the most massive exoplanets. We use Atacama LargeMillimeter/submillimeter Array (ALMA) Band 6 observations of embedded disks inthe Perseus star-forming region together with Very Large Array (VLA) Ka-band (9mm) data to provide a robust estimate of dust disk masses from the fluxdensities. Using the DIANA opacity model including large grains, with a dustopacity value of $\kappa_{\rm 9\ mm}$ = 0.28 cm$^{2}$ g$^{-1}$, the median dustmasses of the embedded disks in Perseus are 158 M$_\oplus$ for Class 0 and 52M$_\oplus$ for Class I from the VLA fluxes. The lower limits on the medianmasses from ALMA fluxes are 47 M$_\oplus$ and 12 M$_\oplus$ for Class 0 andClass I, respectively, obtained using the maximum dust opacity value$\kappa_{\rm 1.3mm}$ = 2.3 cm$^{2}$ g$^{-1}$. The dust masses of young Class 0and I disks are larger by at least a factor of 10 and 3, respectively, comparedwith dust masses inferred for Class II disks in Lupus and other regions. Thedust masses of Class 0 and I disks in Perseus derived from the VLA data arehigh enough to produce the observed exoplanet systems with efficienciesacceptable by planet formation models: the solid content in observed giantexoplanets can be explained if planet formation starts in Class 0 phase with anefficiency of $\sim$ 15%. Higher efficiency of $\sim$ 30% is necessary if theplanet formation is set to start in Class I disks.

Dust masses of young disks: constraining the initial solid reservoir for planet formation