几个恒星形成团块中的CS分子激发温度的迭代计算

Presentation on theme: "几个恒星形成团块中的CS分子激发温度的迭代计算"— Presentation transcript:

1 几个恒星形成团块中的CS分子激发温度的迭代计算
国家天文台 王冰如 指导老师：钱磊 副研究员 本工作内容指导老师

2 Outlines Four Massive Star Forming Active Clumps
Assumptions Adopted in Calculation Iterative Calculation

3 Four Massive Star Forming Active Clumps
Caltech Submillimeter Observations Telescope (CSO) 350 μm map Objects Source RA J2000 DEC J2000 Distance (kpc) G 08:59:12.00 -47:29:04.0 1.5 G 09:01:54.30 -47:43:59.0 1.3 G 16:21:02.10 -50:35:15.0 3.6 G 16:40:00.20 -48:51:20.0 1.4

4 Four Massive Star Forming Active Clumps
Data Swedish-ESO 15m Submillimeter Telescope (SEST) CS J = 2-1 line and CS J = 5-4 line 40*40 arssec^2

5 Assumptions Adopted in Calculation
CS molecules are in LTE The CS lines are optically thin The background radiation can be ignore The clumps are extended sources and can fill the main beam

6 Iterative Calculation
Tex: see Goldsmith & Longer, 1999, ApJ, 517, 209 主要目的：消除瑞利金斯极限情形下带来的偏差。在只有两条谱线的情况下进行计算。 CS J = 2-1 : GHz; CS J = 5-4 : GHz

7

8 Tex in Rayleigh-Jeans limit (K)
Tex obtained after iterative calculation (K) ΔTex 10.0 8.6 -1.4 15.0 12.9 -2.1 20.0 17.3 -2.7 25.0 21.7 -3.3 30.0 26.1 -3.9 35.0 30.4 -4.6 40.0 34.8 -5.2 45.0 39.2 -5.8 50.0 43.6 -6.4 60.0 52.3 -7.7 70.0 61.1 -8.9 80.0 69.8 -10.2 90.0 78.6 -11.4 100.0 87.4 -12.6 120.0 104.9 -15.1

9 以上内容见 Water abundance in four of the brightest water sources in the southern sky, Wang, B., Qian, L., Li, D., Pan, Z., RAA, 2016, Vol. 16, No. 3, 39 在此感谢我的各位导师，本文的所有合作者，科学编辑老师以及我不知名的文章的审稿人！ （注意：文中计算有错误！使用的方法和今天讲的一样）

10 谢谢！