Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/5553
Title: Star Formation Activity in the Galactic H II Complex S255-S257
Authors: Ojha, D. K
Samal, M. R
Pandey, A. K
Bhatt, B. C
Ghosh, S. K
Sharma, S
Tamura, M
Mohan, V
Zinchenko, I
Keywords: Dust, extinction;Galaxies;Star clusters: general;H II regions;Infrared: ISM;ISM: individual objects (S255);Radio continuum: ISM;Stars: formation
Issue Date: 10-Sep-2011
Publisher: IOP Publishing
Citation: The Astrophysical Journal, Vol. 738, No. 2, 156
Abstract: We present results on the star formation activity of an optically obscured region containing an embedded cluster (S255-IR) and molecular gas between two evolved H II regions, S255 and S257. We have studied the complex using optical and near-infrared (NIR) imaging, optical spectroscopy, and radio continuum mapping at 15 GHz, along with Spitzer-IRAC results. We found that the main exciting sources of the evolved H II regions S255 and S257 and the compact H II regions associated with S255-IR are of O9.5-B3 V nature, consistent with previous observations. Our NIR observations reveal 109 likely young stellar object (YSO) candidates in an area of ~4farcm9 × 4farcm9 centered on S255-IR, which include 69 new YSO candidates. To see the global star formation, we constructed the V – I/V diagram for 51 optically identified IRAC YSOs in an area of ~13' × 13' centered on S255-IR. We suggest that these YSOs have an approximate age between 0.1 and 4 Myr, indicating a non-coeval star formation. Using spectral energy distribution models, we constrained physical properties and evolutionary status of 31 and 16 YSO candidates outside and inside the gas ridge, respectively. The models suggest that the sources associated with the gas ridge are younger (mean age ~1.2 Myr) than the sources outside the gas ridge (mean age ~2.5 Myr). The positions of the young sources inside the gas ridge at the interface of the H II regions S255 and S257 favor a site of induced star formation.
Description: Open Access
URI: http://hdl.handle.net/2248/5553
???metadata.dc.rights???: © IOP Publishing
???metadata.dc.relation.uri???: http://iopscience.iop.org/0004-637X/738/2/156/
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