We study the physical and chemical properties of the molecular clump hosting a young stellar cluster, IRAS 20160+3636, which is believed to have formed via the “collect and collapse” process. Physical parameters of the UC Hii region associated with the embedded cluster are measured from the radio continuum observations. This source is found to be a typical Galactic UC Hii region, with a B0.5 type exciting star, if it is ionized by a single star. We derive a CN/HCN abundance ratio larger than 1 over this region, which may suggest that this clump is being affected by the UV radiation from the Hii region.

Abstract
1. INTRODUCTION
2. OBSERVATIONAL DATA
    2.1. ARO Observations
    2.2. GMRT Observations
3. RESULTS AND DISCUSSION
    3.1. The Ultracompact Hii Region
    3.2. The Molecular Cloud Associated with the UC Hii Region
    3.3. CN and HCN Abundances
4. SUMMARY
REFERENCES

• YOUNG CHOL MINH(Korea Astronomy and Space Science Institute) CORRESPONDING AUTHOR
• KEE-TAE KIM(Korea Astronomy and Space Science Institute)
• CHI-HUNG YAN(Academia Sinica Institute of Astronomy and Astrophysics, Department of Earth Sciences, National Taiwan Normal University)
• YONG-SUN PARK(Astronomy Program, Department of Physics and Astronomy, Seoul National University)
• SEOKHO LEE(Astronomy Program, Department of Physics and Astronomy, Seoul National University, Department of Astronomy and Space Science, Kyung Hee University)
• DHARAM VIL LAL(National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune University Campus)
• TATSUHIKO HASEGAWA(Academia Sinica Institute of Astronomy and Astrophysics)
• X. Z. ZHANG(National Astronomical Observatories of China, Chinese Academy of Sciences)
• YI-JENG KUAN(Department of Earth Sciences, National Taiwan Normal University)