Properties of the high-mass star forming region IRAS 22475+5939

作     者：Xiao-Lan Liu Jun-Jie Wang 

作者机构：National Astronomical Observatories Chinese Academy of Sciences Beijing 100012 China Graduate University of Chinese Academy of Sciences Beijing 100049 China 

出 版 物：《Research in Astronomy and Astrophysics》 (天文和天体物理学研究（英文版）)

年 卷 期：2012年第12卷第7期

页      面：845-856页

核心收录：

学科分类：0709[理学-地质学] 07[理学] 0708[理学-地球物理学] 070401[理学-天体物理] 0825[工学-航空宇航科学与技术] 0704[理学-天文学] 

主　　题：ISM: jets and outflow    ISM: molecular    ISM: kinematical and dy namics    star formation 

摘      要：IRAS 22475＋5939 has been we can still discover new characteristics well studied by previous astronomers, but about it, using the first observations of the lines from CO J=2-1, 13C0 J=2-1 and 13CO J=3-2 by the KOSMA 3m telescope. The mapping of the intensity ratio of 13CO J=3-2 and 13CO J=2-1 shows that the distribution of the temperature has two peaks, neither of which coincide with the IRAS 22475＋5939 source or the center of the HII region, but rather are located at the edge of the HII region. Overlays of the Spitzer IRAC 8 p.m with CO contours indicate that they are associated with each other and that the strongest polycyclic aro- matic hydrocarbon （PAH） emission is at the IRAS 22475＋5939 source position. The IRAS LRS spectrum at 7μm-23 μm and the PHT-s spectrum at 2μm-12μm of the IRAS 22475＋5939 source also exhibit strong PAH emission characteristics in the main PAH bands： The diversity of the PAH family should be responsible for the plateaus in the PAH emission in the PHT-s and IRAS-LRS spectra. Analysis and mod- eling in the infrared bands suggest that IRAS 22475＋5939 is more likely to be a class I young stellar object. Where this is the case, the star is likely to have a tempera- ture of Tefr-9995.8K, mass-15.34Mo, luminosity -1.54×104 L- and age 1.54-104 yr. The model shows that circumstellar disc emission is important for wavelengths between 1 and 10μm, otherwise, the envelope fluctuates for A 〉 10μm. Bipolar outflow is confirmed in the molecular cloud, and the excited star of the HII region could be the driving source of the outflow. High resolution is required fm better results.