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http://dx.doi.org/10.5303/JKAS.2015.48.6.343

SEJONG OPEN CLUSTER SURVEY (SOS) - V. THE ACTIVE STAR FORMING REGION SH 2-255 - 257  

LIM, BEOMDU (Korea Astronomy and Space Science Institute)
SUNG, HWANKYUNG (Department of Astronomy and Space Science, Sejong University)
HUR, HYEONOH (Department of Astronomy and Space Science, Sejong University)
LEE, BYEONG-CHEOL (Korea Astronomy and Space Science Institute)
BESSELL, MICHAEL S. (Research School of Astronomy and Astrophysics, Australian National University, MSO)
KIM, JINYOUNG S. (Steward Observatory, University of Arizona)
LEE, KANG HWAN (Gwacheon National Science Museum)
PARK, BYEONG-GON (Korea Astronomy and Space Science Institute)
JEONG, GWANGHUI (Korea Astronomy and Space Science Institute)
Publication Information
Journal of The Korean Astronomical Society / v.48, no.6, 2015 , pp. 343-355 More about this Journal
Abstract
There is much observational evidence that active star formation is taking place in the Hii regions Sh 2-255 – 257. We present a photometric study of this star forming region (SFR) using imaging data obtained in passbands from the optical to the mid-infrared, in order to study the star formation process. A total of 218 members were identified using various selection criteria based on their observational properties. The SFR is reddened by at least E(B −V ) = 0.8 mag, and the reddening law toward the region is normal (RV = 3.1). From the zero-age main sequence fitting method it is confirmed that the SFR is 2.1 ± 0.3 kpc from the Sun. The median age of the identified members is estimated to be about 1.3 Myr from a comparison of the Hertzsprung-Russell diagram (HRD) with stellar evolutionary models. The initial mass function (IMF) is derived from the HRD and the near-infrared (J, J −H) color-magnitude diagram. The slope of the IMF is about Γ = −1.6 ± 0.1, which is slightly steeper than that of the Salpeter/Kroupa IMF. It implies that low-mass star formation is dominant in the SFR. The sum of the masses of all the identified members provides the lower limit of the cluster mass (169M). We also analyzed the spectral energy distribution (SED) of pre-main sequence stars using the SED fitting tool of Robitaille et al., and confirm that there is a significant discrepancy between stellar mass and age obtained from two different methods based on the SED fitting tool and the HRD.
Keywords
open clusters and associations; individual; Sh 2-255 - 257 (IC 2162) - dust, extinction - stars; luminosity function, mass function;
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