论文标题
氨映射观测值，朝向银河巨大的恒星形成区SH 2-255和SH 2-257
Ammonia mapping observations toward the Galactic massive star-forming region Sh 2-255 and Sh 2-257
论文作者
论文摘要
我们进行了NH $ _3 \（j，k）=（1,1），（2,2），$和$（3,3）$映射观测值，使用Nobama 45-M 45-m的望远镜（Kagoshima telsemia）（Kagoshima apperia telsemiia）（Kagoshima apperia telsemia）（Kagoshima apperia telsemia the Nobemiia Amspect temome and Nobemiia ampere for Nobemia ampecope and sh 2-255 sh 2-255 sh 2-257 sh 2-257 sh 2-257 sh 2-257 sh 2-257（sh）线项目。 NH $ _3 $（1,1）在群集S255 N处具有强度峰值，分布在3 pc $ \ times $ 2 $ 2 pc上，位于两个HII区域之间。来自NH $ _3（2,2）/（1,1）$比率的动力学温度为$ \ sim 35 $ K附近的大型群集S255 IR。这些群集还显示出排放，其大线宽度为$ \ sim $ 3-4 km s $^{ - 1} $。根据报道的数据，我们建议这些区域中的NH $ _3 $气体受S255 IR和S255 N的嵌入式YSO群集的恒星反馈。我们还检测到了在II类Adjocects acecacent acecations sechicects shii ysoseacts sh Hii shs sh 2 2 2 2 2 2 2 2 2 2 2 22的主要气体团块以西的NH $ _3 $（1,1）排放的NH $ _3 $（1,1）。 II级YSO的存在意味着$ \ sim 2 $ 2的星形组，比SH 2-254年轻（$ \ sim 5 $ Myr），因此我们建议西部地区的恒星形成可能会受到较旧的HII地区SH 2-254的影响。
We performed NH$_3\ (J,K)=(1,1),(2,2),$ and $(3,3)$ mapping observations toward the Galactic massive star-forming region Sh 2-255 and Sh 2-257 using the Nobeyama 45-m telescope as a part of the KAGONMA (KAgoshima Galactic Object survey with the Nobeyama 45-metre telescope by Mapping in Ammonia lines) project. NH$_3$ (1,1) has an intensity peak at the cluster S255 N, is distributed over 3 pc $\times$ 2 pc and is located between two HII regions. The kinetic temperature derived from the NH$_3 (2,2)/(1,1)$ ratio was $\sim 35$ K near the massive cluster S255 IR. These clusters also show emission with a large line width of $\sim$ 3-4 km s$^{-1}$. Based on the reported data we suggest that NH$_3$ gas in these regions is affected by stellar feedback from embedded YSO clusters in S255 IR and S255 N. We also detected NH$_3$ (1,1) emission in a region west of the main gas clump at the location of a concentration of Class II YSOs adjacent to the HII regions Sh 2-254. The presence of Class II YSOs implies $\sim$ 2 Myr of star formation, younger than Sh 2-254 ($\sim 5$ Myr), thus we suggest that star formation in the western region could be influenced by the older HII region Sh 2-254.
