Sejong open cluster survey (SOS) - V. The active star forming region Sh 2-255 -- 257

TL;DR

This study investigates the active star-forming region Sh 2-255 -- 257 using multi-wavelength photometry, revealing its distance, age, initial mass function, and properties of its young stellar population.

Contribution

It provides a comprehensive photometric analysis of Sh 2-255 -- 257, including membership identification, distance measurement, age estimation, IMF derivation, and SED analysis, highlighting the dominance of low-mass star formation.

Findings

Distance of 2.1 +/- 0.3 kpc from the Sun.

Median age of about 1.3 Myr for members.

IMF slope of about -1.6, steeper than Salpeter/Kroupa.

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 (R_V = 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 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 Gamma = -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_sun). 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.