论文标题
漫画形成区域的柔软度图：弥漫性离子气体污染还是局部福尔摩斯占主导地位？
The softness diagram for MaNGA star-forming regions: diffuse ionized gas contamination or local HOLMES predominance?
论文作者
论文摘要
我们探索所谓的柔软度图 - 其主要功能是提供电离辐射的硬度 恒星形成区域 - 为了检查热和旧低质量进化的星星（Holmes）是否是重要的贡献者 如先前的漫画数据分析所示，恒星形成区域内的电离。我们使用代码HCM-TEFF来得出电离参数和等效有效温度（T*），采用大型恒星和行星星云（PNE）的模型，并探索柔软度图中的不同发射线，以找出出来的主要原因 观察到的漫画和混乱恒星形成区域样品中柔软性参数的差异。我们发现，当漫画（66％）中，与大型恒星相比，源头的t*> 60 kk的比例比来源更难电离（66％），而当[SII] $λλ$ 6716,6731发射线中使用[SII] $λλ$ 6716,6731发射线时（20％）样品。但是，当使用$ 6584的[NII]排放线时，这两个样本中该方案中各个区域的各个部分均大大减少（在漫画中为20％，混乱中的10％）。这可能表明较低分辨率漫画数据中的弥漫性电离气体（DIG）污染负责人为地增加测得的T* 与福尔摩斯在HII地区的主要作用相反。
We explore the so-called softness diagram -- whose main function is to provide the hardness of the ionizing radiation in star-forming regions -- in order to check whether hot and old low-mass evolved stars (HOLMES) are significant contributors to the ionization within star-forming regions, as suggested by previous MaNGA data analyses. We used the code HCm-Teff to derive both the ionization parameter and the equivalent effective temperature (T*), adopting models of massive stars and planetary nebulae (PNe), and exploring different sets of emission lines in the softness diagram to figure out the main causes of the observed differences in the softness parameter in the MaNGA and CHAOS star-forming region samples. We find that the fraction of regions with a resulting T* > 60 kK, which are supposedly ionised by sources harder than massive stars, is considerably larger in the MaNGA (66%) than in the CHAOS (20%) sample when the [SII] $λλ$ 6716,6731 emission lines are used in the softness diagram. However, the respective fractions of regions in this regime for both samples are considerably reduced (20% in MaNGA and 10% in CHAOS) when the [NII] emission line at $λ$ 6584 is used instead. This may indicate that diffuse ionised gas (DIG) contamination in the lower resolution MaNGA data is responsible for artificially increasing the measured T* as opposed to there being a predominant role of HOLMES in the HII regions.
