Protostars and Planets VI, Heidelberg, July 15-20, 2013
The substellar content of the Orion Nebula Cluster
Drass, Holger (Astronomisches Institut, Bochum, Germany)
Chini, Rolf (Astronomisches Institut, Bochum, GermanyInstituto de Astronomía, Universidad Católica del Norte, Antofagasta, Chile )
Nuernberger, Dieter (Astronomisches Institut, Bochum, Germany)
Bayo, Amelia (Max-Planck-Institute for Astronomy, European Southern Observatory, Santiago, Chile)
Hackstein, Moritz (Astronomisches Institut, Bochum, Germany)
Morales-Calderón, Maria (Centro de Astrobiología, Madrid, Spain)
Hoffmeister, Vera (Astronomisches Institut, Bochum, Germany)
Haas, Martin (Astronomisches Institut, Bochum, Germany)
The Substellar Initial Mass Function (SIMF) of many star-forming regions is still poorly known but the detailed knowledge of its shape will help to distinguish among the substellar formation theories. The Orion Nebula Cluster (ONC) is one of the most extensively studied star forming regions. We here present deep, wide-field JHK observations of the ONC taken with HAWK-I@VLT. These observations extend the IMF into the brown dwarf and free-floating planetary mass regime with unprecedented sensitivity.
To obtain a clean sample of ONC members, we exclude potential background sources with the help of CO extinction maps. Masses are assigned by means of evolutionary tracks in the H vs. J-H Color-Magnitude Diagram (CMD). Besides the well known stellar peak at ~0.25 M_sun we find a pronounced second peak at ~0.04 M_sun in the SIMF and indications for a third rise in the free-floating planetary mass regime.
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