Three-dimensional geometry and dust/gas ratios in massive star-forming regions over the entire LMC as revealed by the IRSF/SIRIUS survey
Three-dimensional geometry and dust/gas ratios in massive star-forming regions over the entire LMC as revealed by the IRSF/SIRIUS survey
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IRSF/SIRIUS 调查揭示了整个 LMC 上大质量恒星形成区域的三维几何结构和尘埃/气体比率
DOI：
10.1093/pasj/psac025
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发表时间：
2022
影响因子：
2.3
通讯作者：
Tsuge Kisetsu
中科院分区：
文献类型：
--
作者：
Furuta Takuya;Kaneda Hidehiro;Kokusho Takuma;Nakajima Yasushi;Fukui Yasuo;Tsuge Kisetsu
我们推导出整个尘埃消光（AV）的大麦哲伦云（LMC）的地图估计在近红外波长的颜色过剩。利用我们最近采用的百分位数方法来评估AV分布沿着视线，我们得到了三维（3D）AV地图的三个大质量恒星形成区的N44，N79和N11的基础上IRSF/SIRIUS点源目录。将3DAV图与三种不同速度分量的氢柱密度N（H）进行了比较，其中一种是LMC盘速度，另两种是低于盘速度的速度。因此，我们得到了一个三维尘埃几何形状表明，气体碰撞正在进行之间的不同速度分量。我们还发现了大质量恒星形成区之间气体碰撞时间的差异，这表明N44，N79和N11的气体碰撞发生在比剑鱼座30晚的时间。此外，发现N44的AV/N（H）的速度分量之间的差异为2倍，而N79和N11的差异不显著。从三维几何结构和AV/N（H）的分析，我们认为N44的大质量星星形成是由大麦哲伦星云和小麦哲伦星云之间的潮汐相互作用的外部触发引起的，而N79和N11的大质量恒星形成则可能是由星系旋臂的气体汇聚和超壳层的膨胀等内部触发引起的。尽管不能排除潮汐相互作用的可能性。
We derive the entire dust extinction (AV) map for the Large Magellanic Cloud (LMC) estimated from the color excess at near-infrared wavelengths. Using the percentile method we recently adopted to evaluateAVdistribution along the line of sight, we derive three-dimensional (3D)AVmaps of the three massive star-forming regions of N44, N79, and N11 based on the IRSF/SIRIUS point source catalog. The 3DAVmaps are compared with the hydrogen column densitiesN(H) of three different velocity components where one is of the LMC disk velocity and the other two are of velocities lower than the disk velocity. As a result, we obtain a 3D dust geometry suggesting that gas collision is ongoing between the different velocity components. We also find differences in the timing of the gas collision between the massive star-forming regions, which indicates that the gas collision in N44, N79, and N11 occurred later than that in 30 Doradus. In addition, a difference of a factor of two inAV/N(H) is found between the velocity components for N44, while a significant difference is not found for N79 and N11. From the 3D geometry andAV/N(H) in each star-forming region, we suggest that the massive star formation in N44 was induced by an external trigger of tidal interaction between the LMC and the Small Magellanic Cloud, while that in N79 and N11 is likely to have been induced by internal triggers such as gas converging from the galactic spiral arm and expansion of a supershell, although the possibility of tidal interaction cannot be ruled out.