EPoS Contribution
EPoS Contribution
Constraining the initial solid reservoir for planet formation

Lukasz Tychoniec
Leiden U, Leiden, NL
In recent years evidence has been building that planet formation starts early, in the first 0.5 Myr. Therefore the physical conditions at the early stages of star formation are crucial to understanding the origin of the planetary systems. We use Atacama Large Millimeter/submillimeter Array (ALMA) observations of embedded disks in Perseus together with existing Very Large Array (VLA) data to provide a robust estimate of disk masses and to compare the Perseus survey of dust masses with other ALMA surveys of young and mature disks. Comparison with ALMA surveys of Orion shows that the Class I disk mass distribution is consistent between the two regions, but that the Class 0 disks are more massive in Perseus than in Orion. This shows that initial cloud conditions can have an important effect on the disk masses and possibly on the outcome of the planet formation. We put the improved disk mass estimates in the context of known exoplanetary systems. The dust masses of disks in Class 0/I are significantly larger than those inferred for Class II disks in other regions. The masses of Class 0 and I disks in Perseus can produce the observed exoplanet systems with efficiencies acceptable by models. The most massive observed exoplanets can still be produced by the most massive Class 0 disks with an efficiency of 15%, higher efficiencies are needed if the planet formation starts in Class I.
Caption: The distribution of masses of exoplanetary systems from the exoplanet.eu database. Shaded areas mark the range of Class 0 (red) and Class I dust disk masses in Perseus measured with the VLA.
Collaborators:
E. van Dishoeck, Leiden U, NL
C. Manara, ESO, DE
G. Rosotti, Leiden U, NL
J. Tobin, NRAO, US
A. Cridland, Leiden U, NL
S. van Terwisga, MPIA, DE
T-H. Hsieh, ASIAA, TW
N. Murillo, RIKEN, JP
Suggested Session: Cores2Disks