The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. I. The Initial Mass Function around S Monocerotis

Details The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. I. The Initial Mass Function around S Monocerotis The Initial Mass Function and Young Brown Dwarf Candidates in NGC 2264. I. The Initial Mass Function around S Monocerotis

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aj....128.1684s&link_type=abstract

The Astronomical Journal, Volume 128, Issue 4, pp. 1684-1693.

Astronomy and Astrophysics

Astronomy

25

Galaxy: Open Clusters And Associations: Individual: Ngc Number: Ngc 2264, Stars: Low-Mass, Brown Dwarfs, Stars: Luminosity Function, Mass Function

Scientific paper

The young open cluster NGC 2264 was observed on 2002 January 6-7 with the CFH12K mosaic CCD on the 3.6 m Canada-France-Hawaii Telescope to investigate the shape of the initial mass function (IMF). In order to select the pre-main-sequence (PMS) members more completely, Chandra X-Ray Observatory archival data were retrieved and used for the identification of X-ray-emitting weak-line T Tauri stars. In addition, the (R-I,V-I) diagram was used to exclude background late-type giants, and a statistical approach was applied to estimate the number of contaminating foreground main-sequence stars. The shape of the IMF of the Chandra field of view is flat between logm=-0.4 and ~-1.0 (m in solar mass units), with a weak signature of a dip near logm=-0.2. The overall shape of the IMF is very similar to those obtained for the Pleiades or the Trapezium. The fraction of disked PMS stars, as noted by Rebull and coworkers, does not show any signature of mass dependency. The age of PMS stars between logm=0 and -1 is 3.1+/-0.5 Myr.

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