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A. Porras (Instituto Nacional de Astrofisica, Mexico.), I. Cruz-Gonzalez (Instituto de Astronomia, Mexico), L. Salas (Instituto de Astronomia, UNAM)
We present a photometric technique to construct the initial mass function (IMF), based on NIR observations, of a sample of young stellar clusters (YSCs) located along the Perseus Arm.
J-H/H-K and J/J-H diagrams are used to reveal their interstellar extinction and richness of PMS stars. Luminosity functions are used to estimate ages of YSCs. Masses are obtained following the method by Meyer 1996, together with Carpenter et al. 1993 empirical relations for WTTS, CTTS and Ae/Be stars.
Mass histograms and analysis of the IMF slope values (\Gamma = d log \Phi (log M*) / d log M*) are discussed. A classification of the YSCs based on stellar density, massive star content and number of PMS stars, and the possible implications on IMF differences are addressed.
This work has been financed by grants IN-501694 and IN-120198 from DGAPA (UNAM) and A. Porras has been supported by a CONACYT (México) scholarship.
The author(s) of this abstract have provided an email address for comments about the abstract: irene@astroscu.unam.mx